https://cmb-s4.uchicago.edu/wiki/api.php?action=feedcontributions&user=Bracine&feedformat=atomCMB-S4 wiki - User contributions [en]2022-08-11T14:58:33ZUser contributionsMediaWiki 1.34.2https://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10463Speakers bureau talks list2020-01-25T00:43:42Z<p>Bracine: /* Past talks */</p>
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<div>==Useful links==<br />
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'''[[Speakers Bureau]]'''<br />
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===Proposed talks===<br />
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! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
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===Approved talks===<br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
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| [[Media:myslides.pdf]]<br />
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| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
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| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
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| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
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| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
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| <!--13 Jan 2020 --><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
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| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
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| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
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| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
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Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
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We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
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| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
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| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
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Short abstract:<br />
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CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
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| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
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| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
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| [[Media:myslides.pdf]]<br />
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| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
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===Past talks===<br />
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| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
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| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] <br /> [[File:S4_DESC_meeting_Tucson_2020_Racine_reduced_size.key]] <br />
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|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
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| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
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| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
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| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
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| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
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| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
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| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
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| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
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|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
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|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
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| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
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| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
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| [[Media:]]<br />
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| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
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| [[Media:]]<br />
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| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
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| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
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| [[Media:myslides.pdf]]<br />
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|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:S4_DESC_meeting_Tucson_2020_Racine_reduced_size.key&diff=10462File:S4 DESC meeting Tucson 2020 Racine reduced size.key2020-01-25T00:39:49Z<p>Bracine: </p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10461Speakers bureau talks list2020-01-25T00:39:10Z<p>Bracine: /* Past talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
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===Proposed talks===<br />
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{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
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|}<br />
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===Approved talks===<br />
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{|class="wikitable"<br />
! <!--Announced--><br />
! Date <br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
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<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020 --><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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|-<br />
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|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
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|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
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|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
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<br />
<br />
<br />
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<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
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|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|-<br />
| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] [[File:S4_DESC_meeting_Tucson_2020_Racine_reduced_size.key]] <br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
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|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
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|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
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<br />
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|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
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|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
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<br />
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|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
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|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf&diff=10460File:S4 DESC meeting Tucson 2020 Racine v2.pdf2020-01-25T00:35:48Z<p>Bracine: Bracine uploaded a new version of File:S4 DESC meeting Tucson 2020 Racine v2.pdf</p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10459Speakers bureau talks list2020-01-25T00:33:32Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
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===Proposed talks===<br />
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{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
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|}<br />
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===Approved talks===<br />
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{|class="wikitable"<br />
! <!--Announced--><br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020 --><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
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|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
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| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
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|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
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|-<br />
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| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
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|-<br />
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| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
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|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
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|}<br />
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===Past talks===<br />
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{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|-<br />
| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] <br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10458Speakers bureau talks list2020-01-25T00:31:04Z<p>Bracine: /* Past talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! <!--Announced--><br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020 --><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|-<br />
| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] <br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf&diff=10446File:S4 DESC meeting Tucson 2020 Racine v2.pdf2020-01-17T21:41:07Z<p>Bracine: Bracine uploaded a new version of File:S4 DESC meeting Tucson 2020 Racine v2.pdf</p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10445Speakers bureau talks list2020-01-17T21:34:22Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! <!--Announced--><br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020 --><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10444Speakers bureau talks list2020-01-17T21:34:00Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
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{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
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|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! <!--Announced--><br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
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! style="width: 40%" | Abstract <br />
! Slides<br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
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<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020--><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| <!--13 Jan 2020 --><br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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|-<br />
| <!-- 12 Nov 2019 --><br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:https://cmb-s4.org/wiki/images/S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10435Speakers bureau talks list2020-01-16T23:23:41Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
<br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[https://cmb-s4.org/wiki/images/S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
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|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
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<br />
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|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
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|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
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|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
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|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
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<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10434Speakers bureau talks list2020-01-16T23:23:07Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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===Approved talks===<br />
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{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
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! style="width: 40%" | Abstract <br />
! Slides<br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
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|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
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|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
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|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
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|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
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|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
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| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
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|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
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| [[Media:myslides.pdf]]<br />
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|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
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===Past talks===<br />
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{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
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<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
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<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
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|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
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|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
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|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
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|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
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|-<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
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|-<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
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|-<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
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| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
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|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
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|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
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|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
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|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
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| [[Media:myslides.pdf]]<br />
<br />
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|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
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<br />
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|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
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|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
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|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
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|- <br />
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| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
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| [[Media:Moriond2018_Buza.pdf]]<br />
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|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
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|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
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|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
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<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf&diff=10433File:S4 DESC meeting Tucson 2020 Racine v2.pdf2020-01-16T23:21:08Z<p>Bracine: </p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10432Speakers bureau talks list2020-01-16T23:19:48Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[Media:S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
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|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
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|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
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|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
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<br />
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|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10431Speakers bureau talks list2020-01-16T23:18:30Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
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{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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===Approved talks===<br />
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{|class="wikitable"<br />
! Announced<br />
! Date <br />
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! Speaker <br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
| [[S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
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<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
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<br />
<br />
<br />
|-<br />
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| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
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|}<br />
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===Past talks===<br />
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{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
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|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
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|- <br />
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| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
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|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
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|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10430Speakers bureau talks list2020-01-16T23:17:23Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
<br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
|[[S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10429Speakers bureau talks list2020-01-16T23:16:51Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
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{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
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|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
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|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
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|}<br />
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===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
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|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
|[[https://cmb-s4.org/wiki/images/S4_DESC_meeting_Tucson_2020_Racine_v2.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
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|}<br />
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===Past talks===<br />
<br />
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{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10428Speakers bureau talks list2020-01-15T22:36:35Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
<br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| 22 Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
|[[https://cmb-s4.org/wiki/images/S4_DESC_meeting_Tucson_2020_Racine.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10427Speakers bureau talks list2020-01-15T22:34:11Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
<br />
|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
|[[https://cmb-s4.org/wiki/images/S4_DESC_meeting_Tucson_2020_Racine.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:S4_DESC_meeting_Tucson_2020_Racine.pdf&diff=10426File:S4 DESC meeting Tucson 2020 Racine.pdf2020-01-15T22:32:36Z<p>Bracine: </p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=10425Speakers bureau talks list2020-01-15T22:31:53Z<p>Bracine: /* Approved talks */</p>
<hr />
<div>==Useful links==<br />
<br />
'''[[Speakers Bureau]]'''<br />
<br />
===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! style="width: 50px;" | Venue !! Speaker !! Title/Topic !! Abstract !! Slides <br />
<!-- Generic Template <br />
|- <br />
| Announced date<br />
| 01 Jan 2021 <br />
| Fancypants Conference <br />
| Postdoc McSpeaker <br />
| CMB-S4 strikes back<br />
| In this talk I will present many, many wonderful things about CMB-S4, and the many, many wonderful people who contribute. <br />
| [[Media:myslides.pdf]]<br />
--><br />
<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium on CMB/HEP<br />
| Raphael Flauger<br />
| Searching for Primordial Gravitational Waves with CMB-S4 <br />
| Observations of the cosmic microwave background have been key to our understanding of the early universe. The cosmic microwave background also contains invaluable information about particle physics that can be revealed through precision observations of the polarization anisotropies. In this talk I will review the implications of a detection of primordial gravitational waves from the early Universe and discuss the expected sensitivity for the next generation ground-based CMB experiment CMB-S4.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Marilena Loverde<br />
| Testing Neutrinos with CMB-S4<br />
|Neutrinos remain one of the least understood particles in the standard model. I will describe how a future high-resolution CMB experiment such as CMB-S4 can test a variety of neutrino properties: the neutrino mass, interactions, and in combination with laboratory experiments, point towards the Majorana or Dirac nature of neutrinos.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Joel Meyers<br />
| Light Relics and the Cosmic Microwave Background<br />
| Many well-motivated extensions of the Standard Model of particle physics predict new light degrees of freedom. In many cases, these new light states would have been in thermal equilibrium in the early universe. The extra radiation energy density from such new states would leave a number of imprints in cosmological observables. The temperature and polarization anisotropies of the cosmic microwave background (CMB) on small angular scales are a particularly sensitive probe of the density of light relics. Upcoming CMB experiments will significantly improve sensitivity to the density of light relics, and thereby provide broad and useful constraints on models of new physics. I will discuss the physics of light relics related to the CMB and the sensitivity anticipated from upcoming CMB surveys.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Vera Gluscevic<br />
| Probing dark matter with next-generation CMB experiments<br />
| The next-generation CMB observations from projects such as CMB-S4 will open up new parameter space for exploring interactions of sub-GeV dark matter particles, in regimes largely inaccessible to present-day lab experiments. I will discuss prospects for dark matter searches with CMB-S4 and highlight its complementarity to other experiments.<br />
| [[Media:]]<br />
<br />
|-<br />
| 13 Jan 2020<br />
| 18-21 April 2020<br />
| April APS minisymposium<br />
| Clarence Chang<br />
| CMB-S4 instrumentation<br />
| CMB-S4 is a major focus of the ground based CMB community. Three key science goals driving the technical requirements for CMB-S4 are: 1) searching for primordial gravitational waves resulting from an early period of accelerated expansion (inflation), 2) searching for new light relic particles in the early universe, and 3) providing a legacy survey of nearly half the sky at centimeter to millimeter wavelengths. Crossing critical thresholds for these science topics requires fielding the largest proposed payload of superconducting detectors on multiple telescopes across different sites. I will provide an overview of the CMB-S4 instrumentation plan with particular focus on its superconducting detector technology.<br />
| [[Media:]]<br />
<br />
<br />
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|}<br />
<br />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced<br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 40%" | Abstract <br />
! Slides<br />
<!-- Generic Template <br />
|- <br />
| 25 May 2018<br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
| <br />
| [[Media:myslides.pdf]]<br />
--> <br />
<br />
<br />
|-<br />
| 12 Nov 2019<br />
| Jan 2020<br />
| DESC collaboration meeting<br />
| Benjamin Racine<br />
| Overview of CMB-S4 and LSS synergies<br />
|<br />
|[[Media:S4_DESC_meeting_Tucson_2020_Racine.pdf]] note that this is a draft, and actual talk is a keynote<br />
<br />
<br />
<br />
|-<br />
|<br />
|<br />
| CPAD workshop<br />
| Thomas Cecil<br />
| Development of Large Scale CMB Detector Arrays at Argonne<br />
| The cosmic microwave background (CMB) provides a unique window on the physics of the early Universe probing a variety of fundamental physics such as primordial gravitational waves and neutrino masses. Many of the advances in the field of CMB science have been enabled by advances in detector technology. Ground-based CMB experiments have seen order of magnitude increases in detector count with each subsequent stage with current stage-3 experiments fielding ~10K detectors. In this talk I will provide an overview of CMB detector development to date at Argonne and discuss ongoing efforts focused on developing detectors for post-stage-3 experiments like CMB-S4.<br />
<br />
<br />
<br />
<br />
|-<br />
| <br />
| <br />
| Cosmic Flows, Large-Scale Structure and Visualisation, Stellenbosch, South Africa,<br />
| Elena Pierpaoli (invited)<br />
|<br />
|<br />
|<br />
<br />
<br />
|-<br />
| <br />
| June 2020<br />
| SPIE Yokohama<br />
| Patricio Gallardo<br />
| Stray light analysis and sidelobe calculations for millimeter-wave telescope structure, and baffle optimization<br />
| Long Abstract: <br />
<br />
Stray light and the sidelobes generated by it introduce systematics to millimeter wave telescopes in a variety of ways. Stray light introduces loading on the detector array, impacting mapping speed. The sky projection of the stray light pattern after interacting with the comoving structure produces sidelobes and their projection on low angles introduce scan-synchronous signals. These effects can be simulated and minimized by careful numerical evaluation and optimization.<br />
In this work we present a quantitative ray tracing framework that allows numerical evaluation of baffling strategies to inform the design and optimization of the comoving structure and ground shielding of a millimeter-wave cosmology experiment. We present Zemax models and code to assist the stray light analysis of a large aperture telescope model given a beam prescription for the camera optics, which can be estimated by simulation of the camera optical prescription or measured in the field. This analysis can be used to estimate the on-sky solid angle distribution of stray light (sidelobes). On-sky power metrics can be used to optimize the design of baffling in the telescope structure according to design directives. This implementation does not report polarization, however the method is general enough that it can be expanded in future versions. We provide examples to motivate the study and show early forecasts for CMB-S4. The code to generate the analysis and examples are made publicly available on github for future use.<br />
<br />
<br />
Short abstract:<br />
<br />
We present the implementation of a method to estimate the sidelobe pattern of a millimeter wave telescope. This method can be used to quantify the amount of light spilled at warm reflective surfaces (or the cold sky) and enables optimization of baffling structures and ground shields to follow design directives. We release code that runs Zemax calculations using a 3D model of the telescope comoving structure plus ground screen for optimization and a prescription for spillover from the camera beam. This code was used in the design of the baffling strategy of the Simons Observatory, and is currently being used to design baffling and ground shielding strategies for CMB-S4, a next generation cosmic microwave background experiment.<br />
|<br />
<br />
<br />
<br />
<br />
<br />
<br />
|-<br />
| <!-- 13 Nov 2019 --><br />
| Jun 2020<br />
| SPIE ATI, Yokohama<br />
| Benjamin Schmitt<br />
| Early Project Design and Development Update for the CMB Stage 4 Small Aperture Telescopes Program (poster)<br />
| The next decade of ground-based Cosmic Microwave Background (CMB) experiments will look to push the boundaries of our ability to probe key characteristics of the primordial Universe. Among the greatest near-term goals within the scientific scope of next-generation CMB platforms is to test the inflationary theory of the early Universe by constraining the tensor-scalar ratio “r” via the search for primordial B-mode polarization. Building off of the heritage of the past few decades of ground-based telescopes dedicated to CMB research, the CMB “Stage 4” (CMB-S4) program will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5 meter class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and at the Amundsen-Scott South Pole Station in Antarctica. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. This talk will provide an overview of the current status of the early design, deployment, and operations plan of the CMB-S4 Small Aperture Telescope program.<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 14-19 June 2020 <br />
| SPIE Astronomical Telescopes + Instrumentation 2020, Yokohama<br />
| Amy Bender<br />
| The CMB-S4 experiment: project overview and status<br />
| Long abstract:<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. The forecasted ultra-deep measurements of the CMB polarization will constrain the amplitude of primordial gravitational waves at level that will either detect this unique signature of an inflationary epoch or exclude entire classes of theoretical models. Another driving scientific goal of CMB-S4 is to map out fluctuations in the matter density of the cosmos using both gravitational lensing of the CMB and the secondary CMB anisotropy created by galaxy clusters, informing models of dark energy and modified gravity. Finally, the planned large-area survey of the sky will provide an unprecendented millimeter-wavelength data set for studies of astronomical phenomena, including an new window into time-variable sources and events. The significant opportunities provided by CMB-S4 also bring significant technological challenges. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large sky area) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
<br />
<br />
<br />
Short abstract:<br />
<br />
CMB-S4 is a planned ground-based experiment with scientific impacts reaching from transformative measurements of the cosmic microwave background (CMB) to a deep legacy millimeter-wavelength dataset covering a large fraction of the sky. To meet its ambitious goals, CMB-S4 plans to have small-aperture (0.55-meter) and large-aperture (6-meter) telescopes located both in the Atacama desert (to access a large fraction of the sky) and at the South Pole (for targeted deep-field observations). A total of over 500,000 superconducting detectors will be distributed across these telescopes, enabling a necessary leap in sensitivity. In this talk, I will give an overview of CMB-S4. I will highlight some of its scientific opportunities as well as presenting the driving technical considerations and the current experimental design. <br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
|<br />
| <br />
| AAS Jan<br />
| Dan Grin<br />
| S4 ultralight axion kSZ constraints<br />
|<br />
|<br />
<br />
<br />
<br />
<br />
|-<br />
| 14 Sep 2019<br />
| May 2020<br />
| The Accelerating Universe: Physics and Astrophysics of Dark Energy and Gravitation, Garching<br />
| Elena Pierpaoli<br />
| CMB-S4 overview<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|-<br />
| <!--14 Sep 2019--> <br />
| 16-19 Dec 2019<br />
| B-modes from space, Garching<br />
| Benjamin Schmitt<br />
| Project Design and Development Update for the BICEP Array and CMB Stage 4 Small Aperture Telescope Programs<br />
| Measurement of the polarized Cosmic Microwave Background (CMB) over the past few decades has enabled precision probes of the evolutionary history, composition, and dynamics of the primordial Universe. Next-generation CMB experiments will extend this scientific reach, notably allowing for tests of the inflationary theory of the early Universe, driven through constraints on the tensor-scalar ratio "r" via the search for primordial B-mode polarization. The BICEP Array telescope program will target observation of B-modes at large angular scales, building on constraints already placed by the BICEP/Keck program. BICEP Array is a CMB "Stage 3" class instrument and comprises four BICEP3-class receivers which will operate in conjunction with BICEP3 at 30/40, 95, 150, and 220/270 GHz. The 30/40 GHz receiver will be deployed to the Amundsen-Scott South Pole Station during the 2019/2020 Austral summer. With all receivers deployed, BICEP Array will measure primordial gravitational waves to a precision of σ(r) between 0.002 and 0.004 after a full three years of observations, with over 30,000 detectors on the sky. The BICEP Array experiment will, along with several other CMB telescopes currently in development, serve as a pathfinder experiment for the next-generation of CMB polarization experiments, called CMB "Stage 4" (CMB-S4). The CMB-S4 program is set to lead the global development of next-generation CMB telescope platforms over the next decade, and will lead a worldwide effort to probe the CMB temperature and polarization with unprecedented precision. CMB-S4 will deploy several new large aperture telescopes and approximately eighteen new small aperture telescopes (0.5m class refracting telescopes currently in development) across sites in the Atacama Desert of Northern Chile and the South Pole. With its enormous increase in sensitivity, CMB-S4 will cross critical thresholds for testing inflation, as well as advancing a range of broader science goals. In this talk, I will provide an overview of the current status of the design, integration, and deployment of the first BICEP Array receiver, as well as a summary of the technology development profile for the CMB-S4 small aperture telescope program.<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable" style="width: 90%"<br />
|-<br />
! <!--Announced--> <br />
! Date <br />
! style="width: 50px" | Venue <br />
! Speaker <br />
! Title/Topic <br />
! style="width: 350px" | Abstract <br />
! Slides<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 15-20 Dec 2019 <br />
| Texas Symposium on Relativistic Astrophysics<br />
| Levon Pogosian<br />
| Expected CMB-S4 constraints on birefringence and primordial magnetic fields<br />
| <br />
| [[Media:Pogosian_Dec18_2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!--31 July 2019--><br />
| 11-17 Aug 2019<br />
| Rencontres du Vietnam Cosmology<br />
| Benjamin Saliwanchik<br />
| Cosmology with the Highly Redshifted 21cm Line<br />
| (Can tie in CMB cross-correlations into talk, and give CMB-S4 a mention)<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--15 May 2019 --><br />
| 23-27 Sep 2019<br />
| Italian Physics Society <br />
| Maurizio Tomasi<br />
| Status and prospects for CMB<br />
| (Will dedicate a few slides to CMB-S4) <br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <!--7 Jun 2019--><br />
| 11-17 Aug 2019 <br />
| Rencontres du Vietnam Cosmology<br />
| Francois Bouchet<br />
| Invited talk on current cmb status/planck, prospects for CMB-S4<br />
| <br />
| [[Media:FRB-QuyNhon-CMB-future.pdf]]<br />
<br />
<br />
|- <br />
| <!-- 7 Jun 2019 --><br />
| 6-8 August 2019 <br />
| 12th Great Lakes Cosmology Workshop<br />
| Tom Crawford<br />
| Current and Upcoming Ground-based Cosmic Microwave Background Experiments <br />
| Observations of the cosmic microwave background (CMB) form the backbone of our understanding of the formation and evolution of the Universe. In this talk, I will review the state of the field of post-Planck ground-based CMB observations, discuss some of the most exciting science that can be explored with current and upcoming ground-based CMB experiments, and introduce some of the experiments being designed and fielded to pursue those scientific goals.<br />
| [[Media:Crawford glcw 2019.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <!-- 12 Jan 2019 --><br />
| 13-16 April 2019<br />
| APS April Meeting, Devner<br />
| Nils Halverson <br />
| 12 minutes on CMB-S4<br />
| CMB-S4 is a next-generation ground-based cosmic microwave<br />
background (CMB) experiment consisting of dedicated telescopes<br />
equipped with highly sensitive superconducting cameras operating at<br />
multiple sites. CMB-S4 will provide a dramatic leap forward in our<br />
understanding of the fundamental nature of space and time and the<br />
evolution of the Universe. The science goals of CMB-S4 include<br />
illuminating cosmic inflation, measuring the sum of neutrino masses,<br />
searching for relativistic relics in the early universe, characterizing dark<br />
energy and dark matter, and mapping the matter distribution in the<br />
universe. These goals require measurements with unprecedented<br />
sensitivity and control of systematic errors. To address this challenge, the<br />
CMB community has come together to advocate a single comprehensive<br />
“Stage-4” experiment, called CMB-S4, which has been endorsed by the<br />
2014 report of the Particle Physics Project Prioritization Panel (P5)<br />
“Building for Discovery,” and the 2015 NAS/NRC report "A Strategic<br />
Vision for NSF Investments in Antarctic and Southern Ocean Research."<br />
| [[Media:CMB-S4_talk_APS_CMB_MiniSymposium_2019-04-15v2.pptx]]<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Marius Millea<br />
| CMB-S4 constraints on neutrinos and neutrino like particles<br />
| <br />
| [[https://cmb-s4.org/wiki/images/Aas_seattle_2019-expanded.pdf]]<br />
|<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Aurelien Fraisse<br />
| CMB Facilities and Instruments in the 2020s, and Beyond<br />
| A new generation of extremely sensitive experiments will extend precision measurements of the Cosmic Microwave Background (CMB) anisotropies on large angular scales in polarization, and on arcminute scales in intensity and polarization. The complementary capabilities of ground-based, orbital and sub-orbital balloon borne observatories will provide surveys of the polarized mm-wave sky of with unprecedented sensitivity, fidelity, and spectral resolution, enabling an improved understanding of Galactic emission necessary to realize the scientific potential of the CMB. In this talk we will briefly describe the observational programs underway in the coming decade.<br />
| [[Media:AAS_Fraisse.pdf]] [[Media:AAS_Fraisse.key]]<br />
|<br />
<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Emmanuel Schaan<br />
| Growth of structure from joint analyses of cosmic microwave background and large-scale structure data<br />
| I will describe CMB lensing measurements from current and upcoming CMB experiments. In combination with large-scale structure observables such as clustering and lensing, these will probe the growth of structure over a wide range of redshifts, thus constraining the properties of dark energy and the neutrino masses. Furthermore, CMB lensing measurements can help reduce large-scale structure systematics, such as shear calibration in galaxy lensing.<br />
| [[https://cmb-s4.org/wiki/images/AAS_schaan_talk1.pdf]]<br />
|<br />
<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Lindsey Bleem<br />
|The SZ Galaxy Cluster Sample and other Legacy Products from the CMB-S4 Experiment<br />
| The next generation CMB-S4 experiment will conduct a multifrequency (40-270 GHz) survey of ~40% of the sky at an unprecedented combination of depth and resolution, reaching depths of a few uK-arcmin (~100s uJy) at arcmin-scale resolution in the higher frequency channels. These data will be a tremendous resource for the astronomical community: the deep multifrequency maps will enable the identification of a mass-limited sample of >100,000 galaxy clusters via the Sunyaev-Zel’dovich (SZ) effect, a significant number of higher-redshift protoclusters, galactic sources, and over a million active galactic nuclei (AGN) and dusty star-forming galaxies. Beyond these catalogs the individual frequency maps will be combined to produce maps of the matter distribution as traced by gravitational lensing of the cosmic microwave background, hot gas traced via the thermal SZ, galactic dust, and the cosmic infrared background. The observing cadence will also enable time domain science; each location in the footprint will be imaged more than 1000 times over the course of the multiyear survey enabling characterization of near earth objects, AGN lightcurves, and the discovery of transient objects. In this presentation I will highlight these legacy products, particularly focusing on the scientific impact of the new SZ galaxy cluster sample. <br />
| [[https://cmb-s4.org/wiki/images/AAS_Jan19_CMBS4_Survey.key]], [[https://cmb-s4.org/wiki/index.php/File:AAS_Jan19_CMBS4_Survey.pdf]]<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Hill<br />
| Constraining Feedback in Galaxy Formation with Next-Generation CMB Experiments<br />
| The cosmic microwave background (CMB) radiation is a powerful backlight with which to illuminate structure throughout cosmic history. The thermal (tSZ) and kinematic Sunyaev-Zel'dovich (kSZ) effects, sourced by the scattering of CMB photons off free electrons, directly probe the thermal pressure and density of ionized gas, while gravitational lensing of the CMB directly measures the line-of-sight matter density. Measurements of these effects, which have only been robustly detected within the past decade, will transform our understanding of galaxy formation and evolution in upcoming CMB surveys. I will present predictions for the tSZ and kSZ signals of galaxy and cluster populations at various redshifts derived from state-of-the-art cosmological hydrodynamics simulations, with differing implementations of sub-grid feedback physics due to active galactic nuclei and supernovae. While multiple feedback implementations are able to reproduce the stellar properties of galaxies, their predictions for the tSZ and kSZ signals can be distinguished at high significance by upcoming experiments, including CMB-S4. Next-generation CMB surveys will thus provide crucial input to our understanding of galaxy formation, particularly at high redshift, where other probes have limited signal-to-noise. I will conclude by discussing implications of these measurements for the modeling of baryonic effects on the matter power spectrum, which is amongst the largest systematic uncertainties in cosmological constraints derived from weak gravitational lensing data.<br />
| [[https://cmb-s4.org/wiki/images/JCH_AAS_S4.pdf]]<br />
<br />
|-<br />
|<br />
| 7 January 2019<br />
| AAS 223, Seattle<br />
| Colin Bischoff<br />
| The search for primordial gravitational waves with CMB polarization<br />
| Observations of Cosmic Microwave Background B-mode polarization at large angular scales are a uniquely powerful method to search for primordial gravitational waves, such as those predicted by theories of inflation. A major milestone would be to either detect this signature of gravitational waves or else to set an upper limit on the tensor-to-scalar ratio, r < 0.001, which would rule out the most compelling models of large-field inflation. This goal will be met by Stage-3 experiments currently coming online, the CMB Stage-4 project planned for next decade, as well as new balloon-borne and satellite telescopes. Galactic foregrounds and gravitational lensing of E-mode polarization pose major challenges for these measurements, but are already being addressed by current projects. I will discuss the goals and common design features of experiments targeting the primordial gravitational wave signal, as well as forecasts developed for CMB Stage-4.<br />
| [[Media:20190107_bischoff_aas.pdf]]<br />
<br />
|- <br />
| <br />
| 29 November - 1 December 2018 <br />
| Novel Instrumentation for Fundamental Physics Workshop, Puerto Rico<br />
https://indico.cern.ch/event/748721/<br />
| Clarence Chang<br />
| Update on the ongoing activities<br />
| <br />
| [[Media:Chang_COFI_2018.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 22-24 September 2018<br />
| International Symposium on Cosmology and Ali CMB Polarization Telescope, Shanghai<br />
https://indico.leeinst.sjtu.edu.cn/event/44/overview<br />
| Peter Timbie<br />
| CMB-S4 overview and a general discussion of detector development<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15-18 October 2018<br />
| CMB Foregrounds, Tenerife <br />
http://www.iac.es/congreso/cmbforegrounds18/<br />
| Julian Borrill <br />
| CMB-S4 overview<br />
| <br />
| [[Media:tenerife_cmbs4.pdf]]<br />
<br />
|- <br />
|<br />
| 4-9 November 2018<br />
| 8th KIAS Workshop on Cosmology and Structure Formation<br />
http://home.kias.re.kr/cosmology2018/<br />
| Francois Bouchet <br />
| CMB-S4 overview<br />
| <br />
| [[Media:]]<br />
<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| <br />
| Recontres Du Vietnam <br />
| Raphael Flauger<br />
| Plenary talk, including CMB-S4 <br />
| <br />
| [[Media:]]<br />
|- <br />
|<br />
| 14-21 July, 2018<br />
| COSPAR, Pasadena<br />
| John Carlstrom<br />
| The Next Generation Ground-Based Cosmic Microwave Background Experiment, CMB-S4<br />
| <br />
Measurements of the CMB have driven our understanding of the universe and the physics that govern its evolution from primordial quantum fluctuations to its present state. They provide the foundation for the remarkable 6-parameter cosmological model, ΛCDM, which fits all cosmological data, although there are some tensions that may possibly hint at new physics. Far from being the last word in cosmology, the model raises deep questions: Is Inflation correct? What is its energy scale? What is the dark matter? What is the nature of dark energy? Are there light sterile neutrinos, or other light relics? This talk will describe progress on the next generation ground-based CMB experiment, CMB-S4, that is being designed to have sufficient sensitivity and control of systematics to make breakthroughs in many of these areas, i.e., to cross critical thresholds in parameter values or show that ΛCDM is incomplete.<br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 4-11 July 2018<br />
| ICHEP 2018, Seoul<br />
| Masashi Hazumi <br />
| Plenary talk on CMB cosmology<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
<br />
<br />
|- <br />
| 1 Jun 2018<br />
| 1-7 July 2018 <br />
| Marcel Grossman Meeting <br />
| Carlo Baccigalupi<br />
| The Status of the CMB Stage IV Experiment<br />
| Abstract: The 'Stage-4' ground-based cosmic microwave background (CMB) experiment, CMB-S4, consists of dedicated telescopes equipped with highly sensitive superconducting cameras operating at the South Pole, the high Chilean Atacama plateau, and possibly northern hemisphere sites. CMB-S4 will be designed to cross critical thresholds in testing inflation, determining the number and masses of the neutrinos, constraining possible new light relic particles, providing precise constraints on the nature of dark energy, and testing general relativity on large scales. In this contribution, we review the status of the project.<br />
| [[Media:Carlo_Baccigalupi_S4_MGM15.pdf]]<br />
[[Media:Carlo_Baccigalupi_S4_MGM15.odp]]<br />
<br />
<br />
<br />
<br />
|- <br />
| <br />
| 19 Jun 2018 <br />
| POLAR2018<br />
| John Carlstrom <br />
| Status and Future of Cosmic Microwave Background Measurements from Antarctica <br />
| <br />
| [[Media:E1-2-0023-18-Carlstrom-Posted.pdf]]<br />
<br />
<br />
<br />
|- <br />
| <br />
| 17-22 June 2018<br />
| Workshop: WHIM and Cluster Outskirts: Lost and Found Baryons in the Local Universe, UA-Huntsville<br />
| Jim Bartlett <br />
| Gas Feedback<br />
|<br />
| [[Media:myslides.pdf]]<br />
<br />
<br />
<br />
|- <br />
| 25 May 2018<br />
| 04-08 Jun 2018 <br />
| PASCO, Case Western <br />
| John Ruhl <br />
| Plenary talk on CMB-S4 <br />
| <br />
| [[Media:ruhl_pascos_final.pdf]] <br />
[[Media:Ruhl_pascos_final.key]]<br />
<br />
<br />
<br />
<br />
|- <br />
|<br />
| 15 April 2018 <br />
| AAS<br />
| Brad Benson<br />
| CMB-S4 excerpt from "The Hubble Constant from the Cosmic Microwave Background"<br />
| <br />
| [[media:2018_04_15_Benson_CMB_Hubble_CMBS4_slides.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 17-24 March 2018 <br />
| Rencontres de Moriond: Cosmology<br />
| Victor Buza <br />
| CMB-S4 Performance-Based Constraints On Primordial Gravitational Waves<br />
| <br />
The next-generation ground-based cosmic microwave background experiment, CMB-S4, will achieve new thresholds in the search for the B-mode polarization signature of primordial gravitational waves. To quantify these thresholds, as well as to propose an informed experimental configuration that will reach them, the CMB-S4 forecasting working group has developed a Fisher forecasting machinery targeted towards optimizing tensor-to-scalar parameter constraints in the presence of galactic foregrounds and gravitational lensing of the CMB. In this talk I will describe this framework and explain the uniqueness of this particular approach in basing the forecasts on scalings from actual analyses and multi-year achieved performances of the currently deployed BICEP/Keck series of experiments. In addition, I will detail our work on developing map-level noise simulations, and using various sky models, models of instrumental systematics, and analysis methods to explore the robustness of our findings, which most recently appeared in the CMB-S4 CDT report. Finally, I will talk about employing the Fisher framework in tandem with the simulations work to arrive at the currently proposed CMB-S4 strawman configuration. <br />
<br />
| [[Media:Moriond2018_Buza.pdf]]<br />
<br />
<br />
|- <br />
| 22 Jan 2018<br />
| 18-23 March 2018<br />
| Snowcluster<br />
| Nick Battaglia<br />
| On Cluster Profiles with CMB-S4<br />
| <br />
The next generation cosmic microwave background (CMB) experiment, CMB-S4, will make unprecedented measurements of secondary anisotropies in the CMB. I will focus on observations of the thermal and kinetic<br />
Sunyaev-Zel’dovich (SZ) effects, which will provide new windows into the thermodynamic properties of galaxy groups and clusters. I will<br />
show how we can constrain important baryonic processes, like feedback, that govern group and cluster formation through the high fidelity SZ<br />
profile measurements from CMB-S4. Additionally, I will describe the prospects to constrain fundamental physics from SZ observations and<br />
how to mitigate the modeling uncertainties associated with the baryonic processes that currently limit these constraints.<br />
| [[Media:Battaglia_Snowcluster_2018.pdf]]<br />
[[Media:Battaglia_Snowcluster_2018.key]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 31 Jan 2018 <br />
| CMB in Germany<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
|- <br />
|<br />
| 2 Aug 2017 <br />
| NRAO Futures 2017<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[File:AhmedFutures2017CMB-S4.pdf]]<br />
<br />
|- <br />
|<br />
| 6 Jan 2017 <br />
| B modes from space workshop<br />
| Lloyd Knox<br />
| CMB-S4 update<br />
| <br />
| [[Media:]]<br />
<br />
<br />
|- <br />
|<br />
| 2 Mar 2017 <br />
| SLAC Colloquium<br />
| Suzanne Staggs<br />
| Update following Feb 2017 CMB-S4 meeting<br />
|<br />
| [[file:CMB-and-S4-Staggs-SLAC-20170302-final.pptx]] <br />
<br />
|- <br />
|<br />
| 5 Aug 2016 <br />
| NRAO Futures 2016<br />
| Zeesh Ahmed<br />
| <br />
| <br />
| [[file:AhmedFuturesCMBsummary.pdf]]<br />
<br />
|- <br />
|<br />
| July 2016 <br />
| ICHEP 2016<br />
| Jeff McMahon<br />
| <br />
| <br />
| [[media:McMahon_ICHEP2016.pdf]]<br />
<br />
<br />
<br />
|- <br />
|<br />
| 28 Jan 2016 <br />
| Astronomy and Astrophysics Advisory Committee (AAAC)<br />
| John Carlstrom<br />
| CMB-S4 update<br />
| <br />
| [[file:CarlstromCMB-S4_AAAC_160128.pdf]]<br />
<br />
<br />
<br />
|}</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Simulations_for_Measurement_Requirements&diff=10218UCSD-2019: Cross-Cut: Simulations for Measurement Requirements2019-10-19T19:14:37Z<p>Bracine: /* Noise simulations for PWG */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
* How do we coordinate the production of a unified sky model with enough realism and flexibility for the AWGs?<br />
* What simulations do we need for clusters and what cross-checks will be available with data?<br />
<br />
== Agenda ==<br />
<br />
Please add your name below the agenda if you plan to participate in the session,<br />
contact [[User:Zonca]]<br />
<br />
* 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory<br />
* 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding [[File:exgal_sims.pdf]]<br />
* 5 min - Reijo Keskitalo: Scanning strategy for S4 [https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II Chile deep] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile Chile wide] [https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole Pole deep] [https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II Pole wide]<br />
* 5 min - Ben Racine: Noise simulations for PGW analysis [[:File:noise_sims_for_forecasting.pdf|Sims for PGW]]<br />
* 30 min - Discussion:<br />
** Unified sky model<br />
** How to gather requirements from AWG<br />
** Clusters<br />
** Plans for map-based simulations<br />
<br />
Other participants: Raphael Flauger, Kimmy Wu<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/814488334 Zoom link]<br />
<br />
== Notes ==<br />
<br />
[https://hackmd.io/o1KtRAHXSliAP-sfL73r8A Collaborative note taking on hackMD]<br />
<br />
= Cross-Cut: Simulations for Measurement Requirements =<br />
<br />
[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cross-Cut:_Simulations_for_Measurement_Requirements Link to wiki]<br />
<br />
== Agenda and notes ==<br />
<br />
* 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory<br />
* 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding<br />
* 5 min - Reijo Keskitalo: Scanning strategy for S4<br />
* 5 min - Ben Racine: Noise simulations for PGW analysis<br />
* 25 min - Discussion:<br />
<br />
=== Unified sky model ===<br />
<br />
==== Galactic ====<br />
<br />
* PySM (<code>so_pysm_models</code>) NSIDE 8192 Planck + Gaussian<br />
* MHD: Dust + Synch small patches<br />
* d7 - implement in PySM 3 and increase resolution<br />
* Currently used model up until DSR by the r-forecasting group: <br />
** 00 - Simple Gaussian Sync/Dust with uniform amplitude across the sky<br />
** 01 - PySM base (@zonca has higher nside than 512, to 4096? will get to 8192)<br />
** 02 - PySM extended (@zonca has higher nside than 512, to 4096? will get to 8192)<br />
** 03 - Same as 02 but Hensley/Draine dust model<br />
** 04 - HiDPol dust model (by Tuhin Ghosh)<br />
** 05 - Strong decorrelation model<br />
** 06 - MHD based model from Flauger/Hensley (should swap in &quot;08&quot;: one with more correct synchrotron)<br />
** 07 - Amplitude modulated Gaussian<br />
** 08 - MKD multilayer model from arxiv/1706.04162<br />
** 09 - Vansyngel model as described in arxiv/1611.02577 with multi-frequency extension<br />
* For delensing, we need small scale polarized non-Gaussian Galactic foregrounds. Currently, only 09 has small scale NG.<br />
* discuss: 00 should be replaced with 07? 00 won't be meaningfully used by the large area survey. But it is useful for the deep survey for sanity checks.<br />
* To generalize 08 and 09 into PySM, @zonca has to ask the creator of these models for code/info.<br />
* Q: are there other Galactic models used in S4 outside of the r-forecasting group?<br />
* Check consistency with Planck<br />
* CO lines?<br />
<br />
=== How to gather requirements from AWG ===<br />
<br />
=== Extragalactic + Clusters ===<br />
<br />
* Websky, 1 realization<br />
* validated against planck<br />
* lensing: 1 realization<br />
* radio galaxy sources, catalog input, PySM component could generate map on the fly<br />
* tSZ from Planck, CIB from Herschel and Planck, dusty galaxy count compared to Herschel, stack clusters<br />
<br />
=== Noise ===<br />
<br />
==== Scanning strategy ====<br />
<br />
* https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II<br />
* https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile<br />
<br />
High cadence LAT gives lot of f_sky and daily scans for transients<br />
<br />
* https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole<br />
<br />
Below only done in case of r detection from Deep SAT:<br />
<br />
* https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II<br />
<br />
Jan &amp; Feb we could remove<br />
<br />
Clem has already noise pipeline<br />
<br />
Delensing LAT from Pole??<br />
<br />
==== Noise simulations for PWG ====<br />
<br />
* SAT: start from BK data, fit noise model, just scaling NET and observing time, only data from Pole<br />
* BK NET calculator does not agree with data (in absolute terms), but only relative scaling matters<br />
* Noise calculator is just used for LAT<br />
* SAT: Extrapolating 220 to 270, 95GHz to lower freqs. Will need to be checked when data is available.<br />
* Check POLARBEAR new released performance, use that to scale?<br />
<br />
Delensing '''LAT''' at Pole needs a noise model, maybe scaling SPT??</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Simulations_for_Measurement_Requirements&diff=10196UCSD-2019: Cross-Cut: Simulations for Measurement Requirements2019-10-19T16:59:00Z<p>Bracine: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
* How do we coordinate the production of a unified sky model with enough realism and flexibility for the AWGs?<br />
* What simulations do we need for clusters and what cross-checks will be available with data?<br />
<br />
== Agenda ==<br />
<br />
Please add your name below the agenda if you plan to participate in the session,<br />
contact [[User:Zonca]]<br />
<br />
* 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory<br />
* 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding [[File:exgal_sims.pdf]]<br />
* 5 min - Reijo Keskitalo: Scanning strategy for S4 [https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II Chile deep] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile Chile wide] [https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole Pole deep] [https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II Pole wide]<br />
* 5 min - Ben Racine: Noise simulations for PGW analysis [[:File:noise_sims_for_forecasting.pdf|Sims for PGW]]<br />
* 30 min - Discussion:<br />
** Unified sky model<br />
** How to gather requirements from AWG<br />
** Clusters<br />
** Plans for map-based simulations<br />
<br />
Other participants: Raphael Flauger, Kimmy Wu<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/814488334 Zoom link]<br />
<br />
== Notes ==<br />
<br />
[https://hackmd.io/o1KtRAHXSliAP-sfL73r8A Collaborative note taking on hackMD]</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Noise_sims_for_forecasting.pdf&diff=10195File:Noise sims for forecasting.pdf2019-10-19T16:57:47Z<p>Bracine: </p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Simulations_for_Measurement_Requirements&diff=10194UCSD-2019: Cross-Cut: Simulations for Measurement Requirements2019-10-19T16:57:27Z<p>Bracine: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
* How do we coordinate the production of a unified sky model with enough realism and flexibility for the AWGs?<br />
* What simulations do we need for clusters and what cross-checks will be available with data?<br />
<br />
== Agenda ==<br />
<br />
Please add your name below the agenda if you plan to participate in the session,<br />
contact [[User:Zonca]]<br />
<br />
* 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory<br />
* 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding [[File:exgal_sims.pdf]]<br />
* 5 min - Reijo Keskitalo: Scanning strategy for S4 [https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II Chile deep] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile Chile wide] [https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole Pole deep] [https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II Pole wide]<br />
* 5 min - Ben Racine: Noise simulations for PGW analysis [[File:noise_sims_for_forecasting.pdf]]<br />
* 30 min - Discussion:<br />
** Unified sky model<br />
** How to gather requirements from AWG<br />
** Clusters<br />
** Plans for map-based simulations<br />
<br />
Other participants: Raphael Flauger, Kimmy Wu<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/814488334 Zoom link]<br />
<br />
== Notes ==<br />
<br />
[https://hackmd.io/o1KtRAHXSliAP-sfL73r8A Collaborative note taking on hackMD]</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Component_Separation/Foreground_Cleaning&diff=10183UCSD-2019: Cross-Cut: Component Separation/Foreground Cleaning2019-10-19T16:16:51Z<p>Bracine: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
<br />
<br />
== Agenda ==<br />
<br />
• Introduction: Cora Dvorkin<br />
• [[:File:UCSD_Multicomponent.pdf|Multicomponent model]] : Benjamin Racine (15')<br />
• Hierarchical Generalized Morphological Component Analysis: Sebastian Wagner-Carena (15')<br />
• Machine Learning techniques for component separation: Ben Thorne (15')<br />
• Discussion about a component separation challenge and simulations needed<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:UCSD_Multicomponent.pdf&diff=10182File:UCSD Multicomponent.pdf2019-10-19T16:14:28Z<p>Bracine: </p>
<hr />
<div></div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Component_Separation/Foreground_Cleaning&diff=10181UCSD-2019: Cross-Cut: Component Separation/Foreground Cleaning2019-10-19T16:13:50Z<p>Bracine: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
<br />
<br />
== Agenda ==<br />
<br />
• Introduction: Cora Dvorkin<br />
• [[File:UCSD_Multicomponent.pdf|Multicomponent model]] : Benjamin Racine (15')<br />
• Hierarchical Generalized Morphological Component Analysis: Sebastian Wagner-Carena (15')<br />
• Machine Learning techniques for component separation: Ben Thorne (15')<br />
• Discussion about a component separation challenge and simulations needed<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB&diff=9902UCSD-2019: Analysis/Pipeline Working Group: Low-ell BB2019-10-18T00:08:52Z<p>Bracine: </p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
<br />
# Identify key decisions that must be made (and justified) prior to CD-1,<br />
# Make progress on (or actually make) those decisions, <br />
# Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
# Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
=== Key Issues ===<br />
<br />
* How do we optimize detector allocation across frequency in the face of uncertainty about foreground properties, for both the SATs and the delensing LAT? <br />
* What are the advantages of split bands? How does performance compare to non-split bands?<br />
* Do we need a 20 GHz channel on delensing LAT (for SAT science)<br />
* How well will de-lensing work in practice? <br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
=== What is CD-1? ===<br />
Blatantly copied from [[UCSD-2019: Analysis/Pipeline Working Group: Maps to C_ell | Analysis/Pipeline Working Group: Maps to C_ell]]:<br />
<br />
Background/clarifying questions:<br />
<br />
* What does “by CD-1” mean, and what are the implications for when tools need to be in place and working?<br />
** According to APC white paper (https://arxiv.org/abs/1908.01062), CD-1 is in Q3 of FY2021 (so June 2021?).<br />
*** But according to project office, "Plan [must be] finalized by start of 2020 for delivering...CD-1"<br />
** Working backward from there, any tool that could reasonably influence a CD-1 decision needs to be in place and working by ... ?<br />
** Give an example timeline for an example decision?<br />
<br />
== Agenda ==<br />
<br />
<br />
# Introduction by everyone in the room: who? where? what aspects of low-ell BB interest you? 5 minutes<br />
# Recap of the plan for this session/CD-1 goals [Wu], 3 minutes<br />
# Review of Fisher based S4 forecasting thus far leading to DSR appendix A [Ben/Victor/Raphael], 15 minutes<br />
# Review of Map based S4 forecasting thus far and ideas for next steps [https://docs.google.com/presentation/d/13WQ7t6cyAfchYjKEGw3iuR1U_8QxEC7pJAHmNUmqjXQ Clem], 10 minutes<br />
# Review of forecasting and simulations for Simons Observatory inflation science [Alonso / Errard / Sherwin], 30 minutes<br />
# Plans for working group [all], ~60 minutes<br />
## Forecasting<br />
##* Quantitative comparison of SO and CMB-S4 DSR forecasts<br />
##* Feedback loop between forecasting and data challenges<br />
## Data Challenge simulations<br />
##* More / better foreground models<br />
##* Instrumental systematics<br />
##* Other map non-idealities, i.e. filtering / mode loss<br />
##* Coordination with technical groups on instrument configuration, etc<br />
##* What else needs to be demonstrated for CD1?<br />
## Analysis of Data Challenges<br />
##* Who plans to participate? How do we get more participation?<br />
##* Delensing<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/739724358 Zoom link]<br />
<br />
<br />
== Notes ==</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Tophat_bands_for_Data_Challenge&diff=9262Tophat bands for Data Challenge2019-09-16T21:44:31Z<p>Bracine: </p>
<hr />
<div>''Colin Bischoff -- 2016-11-02, updated 2016-11-04''<br />
<br />
----<br />
<br />
In the process of science book forecasting, we came up with eight bands chosen to split up the four atmospheric windows. These bandpasses are listed in Table 1 of [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160531_fisher/ Victor's 2016-05-31 posting]. I used the center frequencies and fractional bandwidths (&Delta;&nu; / &nu;). I then shifted the 215 GHz band up slightly (to 220 GHz) and widened the 270 GHz band (to 22%) to close a small gap between those bands.<br />
<br />
For each band, I calculated <br />
* relative brightness of a dust-type signal with &beta;<sub>d</sub> = 1.59 and T<sub>d</sub> = 19.5 K; compared to 353 GHz reference frequency<br />
* relative brightness of a synchrotron-type signal with &beta;<sub>sync</sub> = -3.0; compared to 23 GHz reference frequency<br />
<br />
This calculation requires us to specify the convention that we use for our tophat bandpass. I define this tophat to be such that a single-moded antenna (A&Omega; scales as &lambda;<sup>2</sup>) would have uniform response as a function of frequency to a beam-filling Rayleigh-Jeans source. Before we start generating signal simulations, it would be a good idea to check that people generating foreground models agree on this calculation.<br />
<br />
The figure below shows calculated atmospheric brightness spectra (at zenith) for South Pole at 0.5 mm PWV and Atacama at 1.0 mm PWV (both are near median values). Atmospheric spectra are courtesy of Denis Barkats, generated using [https://www.cfa.harvard.edu/~spaine/am/ am]. I plotted the tophat bands on top of these spectra, with the height of each rectangle equal to the band-averaged brightness temperature using the South Pole spectrum. Also shown (in green) are the BICEP2 / Keck Array 150 GHz bandpass and the Keck Array 95 and 220 GHz bandpasses, for comparison. <br />
<br />
The table includes a column that gives the overlap fraction for pairs of bands that split each atmospheric window. This fraction is defined as the ratio between the width of the intersection and the width of the union. Note that it is quite small for the low and high frequency windows, but substantial for the 90 GHz and 150 GHz windows. <br />
<br />
The specific choice of how to split each atmospheric window into two bands was made for the Science Book forecasting effort. The procedure used to come up with the split was to separate two overlapping bands as far as possible while still keeping the calculated per-detector NET within 10-15% of the NET for a detector that spans the full window (see right-hand column of table). There may be room for further optimization of the band definitions, especially with more detailed models of atmosphere and detector performance. It is also likely that they will be changed down the line due to instrumental considerations. For example, if we use multichroic detectors, we would end up with pairs of bands that have little to no overlap. See Adrian's [[Candidate_Frequency_Bands | discussion of split vs staggered bands here]].<br />
<br />
[[File:Tophat_bandpass.png]]<br />
<br />
{| border="1" style="border-collapse: collapse;" cellpadding="5"<br />
! Name !! center [GHz] !! width [GHz] !! dust scale factor <br /> from 353 GHz !! sync scale factor <br /> from 23 GHz !! T<sub>sky</sub> (Pole) [K] !! T<sub>sky</sub> (Atacama) [K] !! overlap fraction !! per-detector NET <br /> [&mu;K sqrt(s)]<br />
|-<br />
| 30 || 30.00 || 9.00 || 0.0059 || 0.3876 || 6.3 || 5.2 || rowspan="2" | 2% || 244<br />
|-<br />
| 40 || 40.00 || 12.00 || 0.0076 || 0.1352 || 12.0 || 8.8 || 306<br />
|-<br />
| 85 || 85.00 || 20.40 || 0.0179 || 0.0104 || 14.5 || 10.9 || rowspan="2" | 37% || 346<br />
|-<br />
| 95 || 95.00 || 22.80 || 0.0210 || 0.0074 || 11.7 || 9.2 || 295<br />
|-<br />
| 145 || 145.00 || 31.90 || 0.0454 || 0.0024 || 10.5 || 10.3 || rowspan="2" | 53% || 350<br />
|-<br />
| 155 || 155.00 || 34.10 || 0.0526 || 0.0021 || 10.9 || 11.7 || 368<br />
|-<br />
| 220 || 220.00 || 48.40 || 0.1368 || 0.0012 || 16.4 || 18.6 || rowspan="2" | 4% || 738<br />
|-<br />
| 270 || 270.00 || 59.40 || 0.2848 || 0.0010 || 21.4 || 24.5 || 1277<br />
|-<br />
| Keck 95 || 95.46 || 25.77 || 0.0212 || 0.0074 || 11.9 || 9.3 || ||<br />
|-<br />
| B2/Keck 150 || 148.92 || 43.52 || 0.0481 || 0.0023 || 11.9 || 12.0 || ||<br />
|-<br />
| Keck 220 || 228.27 || 48.02 || 0.1545 || 0.0012 || 16.9 || 19.1 || ||<br />
|}<br />
<br />
Code used for calculations and plots in this posting: [http://bicep.rc.fas.harvard.edu/cbischoff/tophat_bandpass.py tophat_bandpass.py]</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=9200Simulation and Forecasting Logbook2019-08-30T14:47:49Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
<br />
* '''2019 August 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190829_noise_params_DSR/ Noise parameters for the DC5 DSR-like data challenge] (Ben Racine)<br />
* '''2019 June 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ LAT CDT-STM Noise Levels] (Victor Buza)<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=9199Simulation and Forecasting Logbook2019-08-30T14:47:36Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
<br />
* '''2019 August 29'': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190829_noise_params_DSR/ Noise parameters for the DC5 DSR-like data challenge] (Ben Racine)<br />
* '''2019 June 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ LAT CDT-STM Noise Levels] (Victor Buza)<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8976Simulation and Forecasting Logbook2019-05-28T15:27:15Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8951Simulation and Forecasting Logbook2019-05-13T15:46:51Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8950Simulation and Forecasting Logbook2019-05-13T15:35:23Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress, disregard for now, bug in the masks)] (Ben Racine)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8949Simulation and Forecasting Logbook2019-05-13T15:33:19Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8837Simulation and Forecasting Logbook2019-04-11T18:48:13Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8836Simulation and Forecasting Logbook2019-04-11T18:42:07Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_clossedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8835Simulation and Forecasting Logbook2019-04-11T18:41:27Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 April 11''': [[http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_clossedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search]] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8612Simulation and Forecasting Logbook2019-03-15T23:34:08Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8611Simulation and Forecasting Logbook2019-03-15T23:32:26Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 March 3rd''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8447Simulation and Forecasting Logbook2019-03-11T15:04:26Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 March 3rd''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8407Simulation and Forecasting Logbook2019-03-04T16:36:54Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 March 3rd''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III// CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II// CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8400Simulation and Forecasting Logbook2019-02-28T18:41:09Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 Feb 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III// CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 Jan 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II// CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (B.Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8360Simulation and Forecasting Logbook2019-02-17T22:14:57Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 February 14''': [[Deeper SAT]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (B.Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://users.physics.harvard.edu/~buza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://users.physics.harvard.edu/~buza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://users.physics.harvard.edu/~buza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://users.physics.harvard.edu/~buza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://users.physics.harvard.edu/~buza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://users.physics.harvard.edu/~buza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://users.physics.harvard.edu/~buza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Bracinehttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=8308Simulation and Forecasting Logbook2019-02-04T15:56:40Z<p>Bracine: </p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert)<br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (B.Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effect