https://cmb-s4.uchicago.edu/wiki/api.php?action=feedcontributions&user=Eschaan&feedformat=atomCMB-S4 wiki - User contributions [en]2022-01-26T15:11:22ZUser contributionsMediaWiki 1.34.2https://cmb-s4.uchicago.edu/wiki/index.php?title=UChicago-2020:_Large_Scale_Structure_Surveys&diff=11940UChicago-2020: Large Scale Structure Surveys2020-08-14T03:06:44Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>'''Synergies of Large Scale Structure Surveys with CMB-S4,''' <u>Simone Ferraro</u>, Chihway Chang, and <u>Risa Wechsler </u><br /> We will focus on the synergies of combining tracers of large scale structure as measured at radio through X-ray wavelengths with the wide-field CMB-S4 survey, which will cover ~70% of the sky. We are particularly interested in exploring cosmological analyses that can only be done via the combination of multi-wavelength probes or that are significantly improved through the use of multiple probes (e.g., Nx2 pt, kSZ cosmology, CMB lensing tomography, cosmic shear/WL calibration, cluster cosmology, etc).<br />
<br />
== Connection Details ==<br />
<br />
'''Zoom''': https://fnal.zoom.us/j/97391022720?pwd=QTE4ZzBzcml4MmlZQ1crWjZib0R1dz09<br />
<br />
'''Time/Date''': 10:00am - 11:30am Pacific Time / August 11, 2020<br />
<br />
'''Rapporteurs/Organizers''': Simone Ferraro, Chihway Chang, and Risa Wechsler<br />
<br />
== Agenda ==<br />
* '''Chihway Chang''': [https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing Introduction] (10 min)<br />
* '''Andrina Nicola''': [https://drive.google.com/file/d/1gzCesxfKAkrSP4JXcMiwij7W2LdS_Jz2/view?usp=sharing N x 2pt analysis] (10 min)<br />
* '''Emmanuel Schaan''': [https://cmb-s4.org/wiki/images/Schaan_s4_meeting_20200810.pdf Cosmology with kSZ: baryonic effects in weak lensing] (10 min)<br />
* '''Srini Raghunathan + Chun-Hao To''': [https://docs.google.com/presentation/d/1uLS1tTI3E_rqoMlKhnyWwTQq392pSNChMQw9cZmMPY8/edit?usp=sharing LSS-clusters connection] (10 min)<br />
* '''Marcelo Alvarez, Yuuki Omori, Patricia Larsen''': Correlated simulations update (10 min)<br />
* '''All''': Discussion (30 min)<br />
** Systematics <br />
** Future simulations needs<br />
** Cooperation with external surveys<br />
** Things we've missed<br />
** Your idea here!<br />
<br />
* '''Slide deck:''' https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing<br />
* '''Recording:''' https://drive.google.com/drive/u/3/folders/1eLwWa1SrYkdtdjgi1gYvzINTsj9qIvHy<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UChicago-2020:_Large_Scale_Structure_Surveys&diff=11939UChicago-2020: Large Scale Structure Surveys2020-08-14T03:06:02Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>'''Synergies of Large Scale Structure Surveys with CMB-S4,''' <u>Simone Ferraro</u>, Chihway Chang, and <u>Risa Wechsler </u><br /> We will focus on the synergies of combining tracers of large scale structure as measured at radio through X-ray wavelengths with the wide-field CMB-S4 survey, which will cover ~70% of the sky. We are particularly interested in exploring cosmological analyses that can only be done via the combination of multi-wavelength probes or that are significantly improved through the use of multiple probes (e.g., Nx2 pt, kSZ cosmology, CMB lensing tomography, cosmic shear/WL calibration, cluster cosmology, etc).<br />
<br />
== Connection Details ==<br />
<br />
'''Zoom''': https://fnal.zoom.us/j/97391022720?pwd=QTE4ZzBzcml4MmlZQ1crWjZib0R1dz09<br />
<br />
'''Time/Date''': 10:00am - 11:30am Pacific Time / August 11, 2020<br />
<br />
'''Rapporteurs/Organizers''': Simone Ferraro, Chihway Chang, and Risa Wechsler<br />
<br />
== Agenda ==<br />
* '''Chihway Chang''': [https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing Introduction] (10 min)<br />
* '''Andrina Nicola''': [https://drive.google.com/file/d/1gzCesxfKAkrSP4JXcMiwij7W2LdS_Jz2/view?usp=sharing N x 2pt analysis] (10 min)<br />
* '''Emmanuel Schaan''': [https://cmb-s4.org/wiki/images/Schaan_s4_meeting_20200810.pdf Cosmology with kSZ: baryonic effects in weak lensing] [https://drive.google.com/file/d/13Da1m75HlMQNookMtN3Qh9HDwBjNopi-/view?usp=sharing Cosmology with kSZ: baryonic effects in weak lensing] (10 min)<br />
* '''Srini Raghunathan + Chun-Hao To''': [https://docs.google.com/presentation/d/1uLS1tTI3E_rqoMlKhnyWwTQq392pSNChMQw9cZmMPY8/edit?usp=sharing LSS-clusters connection] (10 min)<br />
* '''Marcelo Alvarez, Yuuki Omori, Patricia Larsen''': Correlated simulations update (10 min)<br />
* '''All''': Discussion (30 min)<br />
** Systematics <br />
** Future simulations needs<br />
** Cooperation with external surveys<br />
** Things we've missed<br />
** Your idea here!<br />
<br />
* '''Slide deck:''' https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing<br />
* '''Recording:''' https://drive.google.com/drive/u/3/folders/1eLwWa1SrYkdtdjgi1gYvzINTsj9qIvHy<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Schaan_s4_meeting_20200810.pdf&diff=11938File:Schaan s4 meeting 20200810.pdf2020-08-14T03:05:28Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UChicago-2020:_Large_Scale_Structure_Surveys&diff=11805UChicago-2020: Large Scale Structure Surveys2020-08-11T04:23:08Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>'''Synergies of Large Scale Structure Surveys with CMB-S4,''' <u>Simone Ferraro</u>, Chihway Chang, and <u>Risa Wechsler </u><br /> We will focus on the synergies of combining tracers of large scale structure as measured at radio through X-ray wavelengths with the wide-field CMB-S4 survey, which will cover ~70% of the sky. We are particularly interested in exploring cosmological analyses that can only be done via the combination of multi-wavelength probes or that are significantly improved through the use of multiple probes (e.g., Nx2 pt, kSZ cosmology, CMB lensing tomography, cosmic shear/WL calibration, cluster cosmology, etc).<br />
<br />
== Connection Details ==<br />
<br />
'''Zoom''': https://fnal.zoom.us/j/97391022720?pwd=QTE4ZzBzcml4MmlZQ1crWjZib0R1dz09<br />
<br />
'''Time/Date''': 10:00am - 11:30am Pacific Time / August 11, 2020<br />
<br />
'''Rapporteurs/Organizers''': Simone Ferraro, Chihway Chang, and Risa Wechsler<br />
<br />
== Agenda ==<br />
* '''Chihway Chang''': Introduction (10 min)<br />
* '''Andrina Nicola''': N x 2pt analysis (10 min)<br />
* '''Emmanuel Schaan''': [https://drive.google.com/file/d/13Da1m75HlMQNookMtN3Qh9HDwBjNopi-/view?usp=sharing Cosmology with kSZ: baryonic effects in weak lensing] (10 min)<br />
* '''Srini Raghunathan + Chun-Hao To''': LSS-clusters connection (10 min)<br />
* '''Marcelo Alvarez, Yuuki Omori, Patricia Larsen''': Correlated simulations update (10 min)<br />
* '''All''': Discussion (30 min)<br />
** Systematics <br />
** Future simulations needs<br />
** Cooperation with external surveys<br />
** Things we've missed<br />
** Your idea here!<br />
<br />
* '''Slide deck:''' https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UChicago-2020:_Large_Scale_Structure_Surveys&diff=11804UChicago-2020: Large Scale Structure Surveys2020-08-11T04:22:50Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>'''Synergies of Large Scale Structure Surveys with CMB-S4,''' <u>Simone Ferraro</u>, Chihway Chang, and <u>Risa Wechsler </u><br /> We will focus on the synergies of combining tracers of large scale structure as measured at radio through X-ray wavelengths with the wide-field CMB-S4 survey, which will cover ~70% of the sky. We are particularly interested in exploring cosmological analyses that can only be done via the combination of multi-wavelength probes or that are significantly improved through the use of multiple probes (e.g., Nx2 pt, kSZ cosmology, CMB lensing tomography, cosmic shear/WL calibration, cluster cosmology, etc).<br />
<br />
== Connection Details ==<br />
<br />
'''Zoom''': https://fnal.zoom.us/j/97391022720?pwd=QTE4ZzBzcml4MmlZQ1crWjZib0R1dz09<br />
<br />
'''Time/Date''': 10:00am - 11:30am Pacific Time / August 11, 2020<br />
<br />
'''Rapporteurs/Organizers''': Simone Ferraro, Chihway Chang, and Risa Wechsler<br />
<br />
== Agenda ==<br />
* '''Chihway Chang''': Introduction (10 min)<br />
* '''Andrina Nicola''': N x 2pt analysis (10 min)<br />
* '''Emmanuel Schaan''': [https://drive.google.com/file/d/13Da1m75HlMQNookMtN3Qh9HDwBjNopi-/view?usp=sharing | Cosmology with kSZ: baryonic effects in weak lensing] (10 min)<br />
* '''Srini Raghunathan + Chun-Hao To''': LSS-clusters connection (10 min)<br />
* '''Marcelo Alvarez, Yuuki Omori, Patricia Larsen''': Correlated simulations update (10 min)<br />
* '''All''': Discussion (30 min)<br />
** Systematics <br />
** Future simulations needs<br />
** Cooperation with external surveys<br />
** Things we've missed<br />
** Your idea here!<br />
<br />
* '''Slide deck:''' https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UChicago-2020:_Large_Scale_Structure_Surveys&diff=11803UChicago-2020: Large Scale Structure Surveys2020-08-11T04:22:28Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>'''Synergies of Large Scale Structure Surveys with CMB-S4,''' <u>Simone Ferraro</u>, Chihway Chang, and <u>Risa Wechsler </u><br /> We will focus on the synergies of combining tracers of large scale structure as measured at radio through X-ray wavelengths with the wide-field CMB-S4 survey, which will cover ~70% of the sky. We are particularly interested in exploring cosmological analyses that can only be done via the combination of multi-wavelength probes or that are significantly improved through the use of multiple probes (e.g., Nx2 pt, kSZ cosmology, CMB lensing tomography, cosmic shear/WL calibration, cluster cosmology, etc).<br />
<br />
== Connection Details ==<br />
<br />
'''Zoom''': https://fnal.zoom.us/j/97391022720?pwd=QTE4ZzBzcml4MmlZQ1crWjZib0R1dz09<br />
<br />
'''Time/Date''': 10:00am - 11:30am Pacific Time / August 11, 2020<br />
<br />
'''Rapporteurs/Organizers''': Simone Ferraro, Chihway Chang, and Risa Wechsler<br />
<br />
== Agenda ==<br />
* '''Chihway Chang''': Introduction (10 min)<br />
* '''Andrina Nicola''': N x 2pt analysis (10 min)<br />
* '''Emmanuel Schaan''': [[https://drive.google.com/file/d/13Da1m75HlMQNookMtN3Qh9HDwBjNopi-/view?usp=sharing | Cosmology with kSZ: baryonic effects in weak lensing]] (10 min)<br />
* '''Srini Raghunathan + Chun-Hao To''': LSS-clusters connection (10 min)<br />
* '''Marcelo Alvarez, Yuuki Omori, Patricia Larsen''': Correlated simulations update (10 min)<br />
* '''All''': Discussion (30 min)<br />
** Systematics <br />
** Future simulations needs<br />
** Cooperation with external surveys<br />
** Things we've missed<br />
** Your idea here!<br />
<br />
* '''Slide deck:''' https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UChicago-2020:_Large_Scale_Structure_Surveys&diff=11802UChicago-2020: Large Scale Structure Surveys2020-08-11T04:22:05Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>'''Synergies of Large Scale Structure Surveys with CMB-S4,''' <u>Simone Ferraro</u>, Chihway Chang, and <u>Risa Wechsler </u><br /> We will focus on the synergies of combining tracers of large scale structure as measured at radio through X-ray wavelengths with the wide-field CMB-S4 survey, which will cover ~70% of the sky. We are particularly interested in exploring cosmological analyses that can only be done via the combination of multi-wavelength probes or that are significantly improved through the use of multiple probes (e.g., Nx2 pt, kSZ cosmology, CMB lensing tomography, cosmic shear/WL calibration, cluster cosmology, etc).<br />
<br />
== Connection Details ==<br />
<br />
'''Zoom''': https://fnal.zoom.us/j/97391022720?pwd=QTE4ZzBzcml4MmlZQ1crWjZib0R1dz09<br />
<br />
'''Time/Date''': 10:00am - 11:30am Pacific Time / August 11, 2020<br />
<br />
'''Rapporteurs/Organizers''': Simone Ferraro, Chihway Chang, and Risa Wechsler<br />
<br />
== Agenda ==<br />
* '''Chihway Chang''': Introduction (10 min)<br />
* '''Andrina Nicola''': N x 2pt analysis (10 min)<br />
* '''Emmanuel Schaan''': [[Cosmology with kSZ: baryonic effects in weak lensing |https://drive.google.com/file/d/13Da1m75HlMQNookMtN3Qh9HDwBjNopi-/view?usp=sharing]] (10 min)<br />
* '''Srini Raghunathan + Chun-Hao To''': LSS-clusters connection (10 min)<br />
* '''Marcelo Alvarez, Yuuki Omori, Patricia Larsen''': Correlated simulations update (10 min)<br />
* '''All''': Discussion (30 min)<br />
** Systematics <br />
** Future simulations needs<br />
** Cooperation with external surveys<br />
** Things we've missed<br />
** Your idea here!<br />
<br />
* '''Slide deck:''' https://docs.google.com/presentation/d/19_5iFfVxFRBsrKv6FAKtxh6kmyOdxcdfnE6UEhJvv6c/edit?usp=sharing<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Cross-correlations_and_Complimentarity_for_LSS&diff=11144LBNL-2020: Cross-correlations and Complimentarity for LSS2020-04-01T18:28:52Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>== Connection Details ==<br />
<br />
'''Zoom''': https://lbnl.zoom.us/j/189656154<br />
<br />
'''Time''': 12:30pm - 1:30pm Pacific Time<br />
<br />
'''Monitor and Scribe''': Simone Ferraro<br />
<br />
== Agenda ==<br />
* '''Simone Ferraro''': Introduction<br />
* '''Blake Sherwin''': Prospects and challenges for S4 lensing cross-correlation cosmology [[File:xcorr2020.pdf]]<br />
* '''Emmanuel Schaan''': Halo energetics and baryon effects with kSZ [https://cmb-s4.org/wiki/images/Talk_s4_meeting_march2020_schaan.pdf slides]<br />
* '''Marcelo Alvarez''': Correlated LSS and CMB simulations [https://cmb-s4.org/wiki/images/Cmb_x_lss_sims.pdf slides]<br />
* '''All''': discussion about joint work with external surveys (DESI, LSST, ...)<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Talk_s4_meeting_march2020_schaan.pdf&diff=11143File:Talk s4 meeting march2020 schaan.pdf2020-04-01T18:27:06Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Cross-correlations_and_Complimentarity_for_LSS&diff=11142LBNL-2020: Cross-correlations and Complimentarity for LSS2020-04-01T18:25:35Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>== Connection Details ==<br />
<br />
'''Zoom''': https://lbnl.zoom.us/j/189656154<br />
<br />
'''Time''': 12:30pm - 1:30pm Pacific Time<br />
<br />
'''Monitor and Scribe''': Simone Ferraro<br />
<br />
== Agenda ==<br />
* '''Simone Ferraro''': Introduction<br />
* '''Blake Sherwin''': Prospects and challenges for S4 lensing cross-correlation cosmology [[File:xcorr2020.pdf]]<br />
* '''Emmanuel Schaan''': Halo energetics and baryon effects with kSZ [[File:talk_s4_meeting_march2020_schaan.pdf]]<br />
* '''Marcelo Alvarez''': Correlated LSS and CMB simulations [https://cmb-s4.org/wiki/images/Cmb_x_lss_sims.pdf slides]<br />
* '''All''': discussion about joint work with external surveys (DESI, LSST, ...)<br />
<br />
== Notes ==<br />
<br />
Real-time notes on [https://docs.google.com/document/d/1fAU8F_yX0T2-cyLixeDJqnWQBHWWcEDLkpNKU3tZYHM/edit?usp=sharing this Google doc].</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Ksz_matter_powerspectrum.pdf&diff=10537File:Ksz matter powerspectrum.pdf2020-03-05T16:31:47Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Joint_Probes_%26_Cross-Correlations&diff=10168UCSD-2019: Cross-Cut: Joint Probes & Cross-Correlations2019-10-19T15:34:36Z<p>Eschaan: /* 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 />
* Define the set of highest-priority cross-correlations<br />
* Determine if more simulation inputs are needed to express the science output of those cross-correlations, and define a schedule and personnel for such simulations<br />
<br />
<br />
== Agenda ==<br />
<br />
* Introduction: Simone Ferraro (10 min)<br />
* kSZ cosmology: Mat Madhavacheril (10 min) [[File:Ksz_mm.pdf]]<br />
* Cluster energetics: Emmanuel Schaan (10 min) [[File:ksztsz_schaan_s4_public.pdf]] [[File:Ksztsz_schaan_s4.key]]<br />
* Lensing cross correlations: Yuuki Omori (10 min)<br />
* Discussion<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Ksztsz_schaan_s4_public.pdf&diff=10167File:Ksztsz schaan s4 public.pdf2019-10-19T15:34:17Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Joint_Probes_%26_Cross-Correlations&diff=10166UCSD-2019: Cross-Cut: Joint Probes & Cross-Correlations2019-10-19T15:33:36Z<p>Eschaan: /* 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 />
* Define the set of highest-priority cross-correlations<br />
* Determine if more simulation inputs are needed to express the science output of those cross-correlations, and define a schedule and personnel for such simulations<br />
<br />
<br />
== Agenda ==<br />
<br />
* Introduction: Simone Ferraro (10 min)<br />
* kSZ cosmology: Mat Madhavacheril (10 min) [[File:Ksz_mm.pdf]]<br />
* Cluster energetics: Emmanuel Schaan (10 min) [[File:ksztsz_schaan_s4.pdf]] [[File:Ksztsz_schaan_s4.key]]<br />
* Lensing cross correlations: Yuuki Omori (10 min)<br />
* Discussion<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Joint_Probes_%26_Cross-Correlations&diff=10165UCSD-2019: Cross-Cut: Joint Probes & Cross-Correlations2019-10-19T15:32:28Z<p>Eschaan: /* 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 />
* Define the set of highest-priority cross-correlations<br />
* Determine if more simulation inputs are needed to express the science output of those cross-correlations, and define a schedule and personnel for such simulations<br />
<br />
<br />
== Agenda ==<br />
<br />
* Introduction: Simone Ferraro (10 min)<br />
* kSZ cosmology: Mat Madhavacheril (10 min) [[File:Ksz_mm.pdf]]<br />
* Cluster energetics: Emmanuel Schaan (10 min) [[File:ksztsz_schaan_s4.pdf]] [[File:Ksztsz_schaan_s4_public.key]] [[File:Ksztsz_schaan_s4.key]]<br />
* Lensing cross correlations: Yuuki Omori (10 min)<br />
* Discussion<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Ksztsz_schaan_s4.key&diff=10164File:Ksztsz schaan s4.key2019-10-19T15:32:20Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Joint_Probes_%26_Cross-Correlations&diff=10156UCSD-2019: Cross-Cut: Joint Probes & Cross-Correlations2019-10-19T14:51:02Z<p>Eschaan: /* 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 />
* Define the set of highest-priority cross-correlations<br />
* Determine if more simulation inputs are needed to express the science output of those cross-correlations, and define a schedule and personnel for such simulations<br />
<br />
<br />
== Agenda ==<br />
<br />
* Introduction: Simone Ferraro (10 min)<br />
* kSZ cosmology: Mat Madhavacheril (10 min)<br />
* Cluster energetics: Emmanuel Schaan (10 min) [[File:ksztsz_schaan_s4.pdf]] [[File:Ksztsz_schaan_s4_public.key]]<br />
* Lensing cross correlations: Yuuki Omori (10 min)<br />
* Discussion<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Ksztsz_schaan_s4_public.key&diff=10155File:Ksztsz schaan s4 public.key2019-10-19T14:50:00Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Joint_Probes_%26_Cross-Correlations&diff=10153UCSD-2019: Cross-Cut: Joint Probes & Cross-Correlations2019-10-19T07:46:01Z<p>Eschaan: /* 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 />
* Define the set of highest-priority cross-correlations<br />
* Determine if more simulation inputs are needed to express the science output of those cross-correlations, and define a schedule and personnel for such simulations<br />
<br />
<br />
== Agenda ==<br />
<br />
* Introduction: Simone Ferraro (10 min)<br />
* kSZ cosmology: Mat Madhavacheril (10 min)<br />
* Cluster energetics: Emmanuel Schaan (10 min) [[File:ksztsz_schaan_s4.pdf]]<br />
* Lensing cross correlations: Yuuki Omori (10 min)<br />
* Discussion<br />
<br />
== Remote attendance ==<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Ksztsz_schaan_s4.pdf&diff=10152File:Ksztsz schaan s4.pdf2019-10-19T07:45:37Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Maps_to_Other_Statistics&diff=10020UCSD-2019: Analysis/Pipeline Working Group: Maps to Other Statistics2019-10-18T18:32:00Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
Background: this working group covers a remarkably broad area of science targets and topics, although none of them are design-driving, primary science goals. Scientifically, it can cover science topics including neutrino mass, structure growth and dark energy / modified gravity, reionization, baryonic physics, and other topics. In terms of measurements covered by this group, they include lensing power spectra and cross-correlations, cluster cosmology, SZ cross-correlations and higher point functions, CMB bispectra, and several others.<br />
<br />
In light of this, major goals of our group are to identify and prioritize several key science targets and analyses, and, with our work as part of this group, strengthen and sharpen these S4 science cases. Our work should also inform the efforts of other working groups (for example by exploring mass calibration for the sources group and lensing systematics for BB-delensing).<br />
<br />
To start, one proposal is to focus on a few of the key science targets: neutrino mass (e.g. from lensing), baryonic physics and reionization. However, we will have a broader discussion on priorities and science targets at the end of the session.<br />
<br />
<br />
== Official Charge Question ==<br />
<br />
* Given plausible CIB models (and galactic foregrounds) at high ell, what frequency coverage (and associated sensitivity) is sufficient to reduce CIB residuals below statistical errors on tSZ and kSZ measurements?<br />
* How severe is the impact of small-scale polarized foregrounds on lensing? (If important, how can we mitigate them?)<br />
* What is the optimal strategy for mitigating temperature lensing foregrounds?<br />
* What are requirements on beam and pointing for sub-percent lensing spectra?<br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
Introductory remarks (Marcelo and Blake)<br />
<br />
<br />
'''Lensing'''<br />
<br />
Foregrounds:<br />
<br />
Emmanuel Schaan: temperature foregrounds in lensing (20+10 mins) [[File:Talk_lensing_foregrounds_cmbs4_schaan.pdf]]<br />
<br />
Kevin Huffenberger: modeling of small-scale non-Gaussian Galactic foregrounds (to characterize lensing bias) (10+5 mins) [[File:Smallscale_foregrounds.pdf]]<br />
<br />
Srini Raghunathan: foregrounds for cluster lensing reconstruction (10+5 mins)<br />
<br />
<br />
Theory:<br />
<br />
Alex van Engelen: baryonic effects for CMB lensing and neutrino mass (10+5 mins)<br />
<br />
<br />
'''SZ'''<br />
<br />
Marcelo Alvarez: constraints on patchy reionization from kSZ (10+5 mins)<br />
<br />
Colin Hill (discussion): CIB cleaning requirements for SZ (10 mins)<br />
<br />
<br />
'''Discussion'''<br />
<br />
Key targets and analyses<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Analysis/Pipeline_Working_Group:_Maps_to_Other_Statistics&diff=10019UCSD-2019: Analysis/Pipeline Working Group: Maps to Other Statistics2019-10-18T18:31:28Z<p>Eschaan: /* Agenda */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
Background: this working group covers a remarkably broad area of science targets and topics, although none of them are design-driving, primary science goals. Scientifically, it can cover science topics including neutrino mass, structure growth and dark energy / modified gravity, reionization, baryonic physics, and other topics. In terms of measurements covered by this group, they include lensing power spectra and cross-correlations, cluster cosmology, SZ cross-correlations and higher point functions, CMB bispectra, and several others.<br />
<br />
In light of this, major goals of our group are to identify and prioritize several key science targets and analyses, and, with our work as part of this group, strengthen and sharpen these S4 science cases. Our work should also inform the efforts of other working groups (for example by exploring mass calibration for the sources group and lensing systematics for BB-delensing).<br />
<br />
To start, one proposal is to focus on a few of the key science targets: neutrino mass (e.g. from lensing), baryonic physics and reionization. However, we will have a broader discussion on priorities and science targets at the end of the session.<br />
<br />
<br />
== Official Charge Question ==<br />
<br />
* Given plausible CIB models (and galactic foregrounds) at high ell, what frequency coverage (and associated sensitivity) is sufficient to reduce CIB residuals below statistical errors on tSZ and kSZ measurements?<br />
* How severe is the impact of small-scale polarized foregrounds on lensing? (If important, how can we mitigate them?)<br />
* What is the optimal strategy for mitigating temperature lensing foregrounds?<br />
* What are requirements on beam and pointing for sub-percent lensing spectra?<br />
* What are the necessary analysis tools to answer these questions?<br />
<br />
== Agenda ==<br />
<br />
Introductory remarks (Marcelo and Blake)<br />
<br />
<br />
'''Lensing'''<br />
<br />
Foregrounds:<br />
<br />
Emmanuel Schaan: temperature foregrounds in lensing (20+10 mins) [File:Talk_lensing_foregrounds_cmbs4_schaan.pdf]]<br />
<br />
Kevin Huffenberger: modeling of small-scale non-Gaussian Galactic foregrounds (to characterize lensing bias) (10+5 mins) [[File:Smallscale_foregrounds.pdf]]<br />
<br />
Srini Raghunathan: foregrounds for cluster lensing reconstruction (10+5 mins)<br />
<br />
<br />
Theory:<br />
<br />
Alex van Engelen: baryonic effects for CMB lensing and neutrino mass (10+5 mins)<br />
<br />
<br />
'''SZ'''<br />
<br />
Marcelo Alvarez: constraints on patchy reionization from kSZ (10+5 mins)<br />
<br />
Colin Hill (discussion): CIB cleaning requirements for SZ (10 mins)<br />
<br />
<br />
'''Discussion'''<br />
<br />
Key targets and analyses<br />
<br />
== Remote attendance ==<br />
<br />
[https://ucsd.zoom.us/j/973144732 Zoom link]<br />
<br />
<br />
== Notes ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Talk_lensing_foregrounds_cmbs4_schaan.pdf&diff=10018File:Talk lensing foregrounds cmbs4 schaan.pdf2019-10-18T18:30:37Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD_2019_Fireslides_1&diff=9918UCSD 2019 Fireslides 12019-10-18T00:59:18Z<p>Eschaan: </p>
<hr />
<div><br />
# Eric Linder, Guilherme Brando - Reconstructing the Primordial Power Spectrum [[File:LinderInflFreeS4.pdf]] <br />
# Aritoki Suzuki - Improving Frequency Multiplexing (fmux) Readout, Work on deployable module [[File:2019_10_17_CMBS4FireSlideFmuxmKSQUIDSuzuki.pdf]]<br />
# Andrea Zonca - PySM 3: Sky models for CMB experiments, [[File:PySM_3.0_fireslide.pdf]]<br />
# Hannes Hubmayr - Microwave Kinetic Inductance Detectors with Negligible 1/f Noise [[File:Hubmayr_mkid_1overf_free.pdf]]<br />
# Zhilei Xu - Galaxy X Compton y-map with ACT and DES [[https://cmb-s4.org/wiki/images/CMB-S4_UCSD_Fireslide_Xu.pdf Slide]]<br />
# Maria Salatino - The AliCPT 1 telescope [[File:CMB-S4_UCSD_Salatino_fireslide.pdf]]<br />
# Kevin Huffenberger - Florida State University activities [[File:FSU_activity.pdf]]<br />
# Brenna Flaug'''h'''er - What you need to know about the DOE Instrumentation Basic Research Needs Process [[File:BRN-Fireslide-flaugher.pdf]] <br />
# Michael Snow - A Big Heat Switch for Big Cryostats [[File:Fireslide_A_Big_Heat_Switch_for_Big_Cryostats.pdf]]<br />
# Grant Teply - UCSD Lab Tour [[File:20191017_lab_tour.pdf]]<br />
# Sebastian Wagner-Carena - Hierarchical Generalized Morphological Component Analysis [[File:HGMCA_fireslide.pdf]]<br />
# Kimmy Wu, Federico Bianchini - SPTpol 500 sq. deg Lensing Power Spectrum and Cosmological Parameters [[File: lens500d_slide_parameters.pdf]]<br />
# Selim Hotinli - Utilising the moving lens effect for cosmology [[File:Hotinli_fire_slide.pdf]]</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Hotinli_fire_slide.pdf&diff=9915File:Hotinli fire slide.pdf2019-10-18T00:58:11Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Speakers_bureau_talks_list&diff=8223Speakers bureau talks list2019-01-16T21:52:16Z<p>Eschaan: /* Past talks */</p>
<hr />
<div>===Proposed talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! Venue !! Speaker !! Title/Topic !! Abstract !! Slides<br />
<!-- Generic Template <br />
|- <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 />
===Approved talks===<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! Venue !! Speaker !! Title/Topic !! Abstract !! 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 />
| 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:]]<br />
<br />
<br />
<br />
|}<br />
<br />
===Past talks===<br />
<br />
<br />
{|class="wikitable"<br />
! Announced !! Date !! Venue !! Speaker !! Title/Topic !! Abstract !! Slides<br />
<br />
<br />
|-<br />
|<br />
| 7 December 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 />
| 7 December 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 December 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 December 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:]]<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:]]<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 />
<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>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:AAS_schaan_talk1.pdf&diff=8222File:AAS schaan talk1.pdf2019-01-16T21:50:53Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7575Princeton-2018: Cosmology with CMB-S42018-09-07T18:12:42Z<p>Eschaan: </p>
<hr />
<div>== Workshop overview ==<br />
<br />
<br />
<br />
'''Workshop Photo:<br />
''' <br /><br />
[[File:CMB-S4_2018-1-photo.jpg|600px]]<br />
<br/><br />
<br />
The Princeton workshop continues a successful series of meetings bringing together the CMB experimental and theoretical community to plan a coordinated, stage-4 ground-based CMB experiment.<br />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 211 655 218<br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<br />
<br />
Slack channel #princeton2018 on the CMB-S4 workspace, or use https://cmb-s4.slack.com/messages/CCMNTUDC1<br />
<br />
== About This Wiki==<br />
<br />
As for previous workshops, we will use this wiki to organize the sessions, to capture the input from them, and to develop next steps. Participants are encouraged to edit the wiki directly, including uploading plots or a few slides.<br />
<br />
Hints for formatting this wiki can be found [https://www.mediawiki.org/wiki/Help:Formatting here]<br />
<br />
== Agenda ==<br />
<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) [[File:Logistics-pton-20180906.pdf]]<br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) [[File:Cmbs4_collaboration.pdf]]<br /> <br />
'''09:05''' DSR Update (John Carlstrom) [[File:DSR-Carlstrom.pdf]]<br /><br />
'''09:25''' Project Update (Jim Yeck) [[File:S4 Princeton Workshop Yeck.pdf]]<br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Lloyd Knox) [[File:DSR_ScienceCouncil_Princeton2018.pdf]]<br /> <br />
'''10:15''' Gravitational Waves & Inflation (Raphael Flauger) [[File: GWPrinceton.pdf]]<br /><br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics (Daniel Green & Joel Meyers) [[File:LightRelics_Meyers_Princeton_S4.pdf]] <br /><br />
'''11:15''' Neutrino Mass (Marilena Loverde & Blake Sherwin) [[File:S4WGNeutrinoMassReport.pdf]]<br /><br />
'''11:30''' Dark Energy & Dark Matter (Vera Gluscevic & Nick Battaglia) [[File:DMDE CMBS4 Princeton2018.pdf]]<br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) [[File:CMB-S4 Galaxy Formation and Evolution (Princeton).pdf]] <br /><br />
'''12:00''' Legacy Catalogs (Lindsey Bleem) [[https://cmb-s4.org/wiki/images/Legacy_catalog_update_princeton_9_6_18.pdf here]]<br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) [[File:TechCouncilPrinceton2018.pdf]] <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) [https://drive.google.com/file/d/1XB3Kt80dbh9qoyvvnppN6RYispp_XFrB/view?usp=sharing Site Presentation PDF]<br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) [[File:LargeTelescopesLargeCryostatsStatusPrincetonV2.pdf]] <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) [[File:SmallTelescopes_Princeton_Thursday_slides.pdf]]<br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) [[File:DetectorsReadout.pdf]]<br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) [[File:S4_DAQ.pdf]] <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) [[File:Data_management_20180906_v1.pdf]] <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Bradford Benson) [[File:IntegrationCommissioningPrinceton2018.pdf]] <br /><br />
'''15:30''' Options (Steve Padin) [[File:OptionsPrincetonV1.pdf]] <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1 [[File:FireSlides_Thursday_post.pdf]]<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) [[File:Morningmarc.pdf]] <br /><br />
'''08:55''' On-sky performance of the CLASS Q-band telescope (John Appel) [[File:CLASS_S4_20180907_final.pdf]]<br /><br />
'''09:05''' SPIDER: an update, with foregrounds. Lots of them. [[File:Cmbs4_aug2018.red.mini.pdf]] (Bill Jones) <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) [[File:BK2018.pdf]] <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) [[File:Planck2018.pdf]] <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) [[File:PrincetonS4_2018V2.pdf]] <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) [[File:BK-SPT3G_forward.pdf]] <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) [[File:SO_plans.pdf]] <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder) [[File:S4_Princeton_holder.pdf]] <br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) [[File:mauskopf_princeton_cmbs4.pdf]] <br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) [[File:2018_09_S4_IntensityMappingCMB.pdf]] <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) [[File:Spherex_cmbs4_2018.pdf]] <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause) [[https://cmb-s4.org/wiki/images/Krause_LSSTxS4_2018.pdf slides_here]]<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) [[File:cmbs4_sep7_18_lidz.pdf]] <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) [[File:CMB-S4_Murray.pdf]]<br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) [[File:Clark_S4_ForegroundModels.pdf]] <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck [[File:Aumont_Princeton_CMB-S4_090718.pdf]] (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) [[File:DvorkinCMBS4.pdf]]<br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) [[File:CMB-S4_princeton18_cyr-racine.pdf]]<br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) [[File:Boddy.pdf]] <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) [[https://cmb-s4.org/wiki/images/Cmb_shear_schaan.pdf slides]]<br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) [[File:NeutrinoXCorrs.pdf]] <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) [[https://cmb-s4.org/wiki/images/HighOrderCorr.pdf slides]]<br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) [[File:Ferraro_s4_princeton.pdf]] <br /><br />
'''15:25''' kSZ cosmology without the cluster optical depth degeneracy (Mathew Madhavacheril) [[File:Madhavacheril_S4kSZ_v1.pdf]] <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2 [[File:FireSlides_Friday_post.pdf]]<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, Matias Zaldarriaga<br /><br />
Contributed material for panel discussion by panelists and audience:<br /><br />
*From George Fuller: [[File:Fuller-CMB-S4.Princeton.pdf]]<br /><br />
*From Roger Blandford:[[File:Cmbs4rdb.pdf]]<br /><br />
*From Chris Carilli: [[File:Carilli-CMBS4.pdf]]<br/><br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** Noise & Forecasting (60 min)<br />
*** 9:00-9:10 r Forecasting Update (Clem Pryke)<br />
***9:10-9:20 small-area survey report from Noise Tiger Team (NTT) (Colin Bischoff)<br />
***9:20-9:40 Discussion<br />
***9:40-9:50 Report from NTT on large-area survey forecasting (Matthew Hasselfield)<br />
***9:50-10:00 Simons Observatory appraoch to TT, TE, EE, phi phi, tSZ, kSZ forecasting (Colin Hill)<br />
***10-10:10 Discussion<br />
** 10:10-11 White Paper Organization<br />
'''11:00-11:30''' ''Coffee Break''<br />
*11:30-1:00 Science Council AWG Breakout Sessions<br />
<br />
* Technical Council:<br />
** Project Planning<br />
<br />
'''10:45''' ''Coffee Break''<br />
<br />
<br />
* Technical Council<br />
** Project Planning (continued)<br />
<br />
'''12:45''' ''Lunch (on your own)''<br />
<br />
'''13:45 onwards''' Rooms available for breakout sessions as required</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:HighOrderCorr.pdf&diff=7574File:HighOrderCorr.pdf2018-09-07T18:12:17Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Princeton-2018:_Cosmology_with_CMB-S4&diff=7525Princeton-2018: Cosmology with CMB-S42018-09-07T14:04:16Z<p>Eschaan: </p>
<hr />
<div>== Workshop overview ==<br />
<br />
The Princeton workshop continues a successful series of meetings bringing together the CMB experimental and theoretical community to plan a coordinated, stage-4 ground-based CMB experiment.<br />
The workshop is supported by Princeton University with a generous contribution from the Kavli Institute for Cosmological Physics.<br />
<br />
This meeting will focus on moving us towards the Decadal Survey and project formation. Each day will have a different flavor:<br />
* Thursday - Collaboration, Project and Decadal Survey Report updates and discussion<br />
* Friday - Broader community building ahead of the Decadal Process<br />
* Saturday - Parallel Science & Technical Council sessions<br />
<br />
== Meeting Info & Registration ==<br />
<br />
[http://phyindico.princeton.edu/indico/event/12/page/0 Official Workshop Website: Registration, Participants, Hotels, Logistics].<br />
<br />
[[File:workshop-map-venue.png]] <br /><br />
Registration begins outside McDonnell A02 at 8 am on Thursday, 6 Sept 2018. <br />
Parking is in lot 21 (see map). <br />
<br />
'''Remote Connection Information:'''<br />
<br />
https://bluejeans.com/ <br /><br />
Meeting ID: 211 655 218<br /><br />
*1.888.240.2560 (US Toll Free)<br />
*1.408.317.9253 (US (Primary, San Jose)) <br />
*1.408.740.7256 (US (San Jose)) <br /><br />
*Global Numbers: https://www.bluejeans.com/numbers<br />
<br />
Slack channel #princeton2018 on the CMB-S4 workspace, or use https://cmb-s4.slack.com/messages/CCMNTUDC1<br />
<br />
== About This Wiki==<br />
<br />
As for previous workshops, we will use this wiki to organize the sessions, to capture the input from them, and to develop next steps. Participants are encouraged to edit the wiki directly, including uploading plots or a few slides.<br />
<br />
Hints for formatting this wiki can be found [https://www.mediawiki.org/wiki/Help:Formatting here]<br />
<br />
== Agenda ==<br />
<br />
<br />
=== Thursday September 6th ===<br />
<br />
'''08:00''' ''Breakfast'' <br />
<br />
'''08:30''' Welcome & Logistics (Suzanne Staggs Herman Verlinde, chair of the Physics Department) [[File:Logistics-pton-20180906.pdf]]<br />
<br />
''' Status & Context'''<br /><br />
'''08:45''' Introduction & Collaboration Update (Julian Borrill) [[File:Cmbs4_collaboration.pdf]]<br /> <br />
'''09:05''' DSR Update (John Carlstrom) [[File:DSR-Carlstrom.pdf]]<br /><br />
'''09:25''' Project Update (Jim Yeck) [[File:S4 Princeton Workshop Yeck.pdf]]<br /><br />
'''09:45''' Q&A<br />
<br />
'''DSR - Science Council''' <br /><br />
'''10:00''' Introduction (Lloyd Knox) [[File:DSR_ScienceCouncil_Princeton2018.pdf]]<br /> <br />
'''10:15''' Gravitational Waves & Inflation (Raphael Flauger) [[File: GWPrinceton.pdf]]<br /><br />
<br />
'''10:30''' ''Coffee Break''<br />
<br />
'''11:00''' Light Relics (Daniel Green & Joel Meyers) [[File:LightRelics_Meyers_Princeton_S4.pdf]] <br /><br />
'''11:15''' Neutrino Mass (Marilena Loverde & Blake Sherwin) [[File:S4WGNeutrinoMassReport.pdf]]<br /><br />
'''11:30''' Dark Energy & Dark Matter (Vera Gluscevic & Nick Battaglia) [[File:DMDE CMBS4 Princeton2018.pdf]]<br /><br />
'''11:45''' Galaxy Formation & Evolution (Marcelo Alvarez & Colin Hill) [[File:CMB-S4 Galaxy Formation and Evolution (Princeton).pdf]] <br /><br />
'''12:00''' Legacy Catalogs (Lindsey Bleem) [[https://cmb-s4.org/wiki/images/Legacy_catalog_update_princeton_9_6_18.pdf here]]<br /><br />
'''12:15''' Q&A<br />
<br />
'''12:30''' ''Lunch & JSAC Event''<br />
<br />
'''DSR - Technical Council'''<br /><br />
'''13:30''' Introduction (McMahon/Vieregg) [[File:TechCouncilPrinceton2018.pdf]] <br /><br />
'''13:45''' Sites & Infrastructure (Kam Arnold, Brad Benson) [https://drive.google.com/file/d/1XB3Kt80dbh9qoyvvnppN6RYispp_XFrB/view?usp=sharing Site Presentation PDF]<br /><br />
'''14:00''' Large Telescopes (Mike Niemack, Steve Padin) [[File:LargeTelescopesLargeCryostatsStatusPrincetonV2.pdf]] <br /><br />
'''14:15''' Small Telescopes (John Kovac, Chao-Lin Kuo, Aikito Kusaka) [[File:SmallTelescopes_Princeton_Thursday_slides.pdf]]<br /><br />
'''14:30''' Detectors & Readout (Clarence Chang, Kent Irwin, Adrian Lee) [[File:DetectorsReadout.pdf]]<br /><br />
'''14:45''' Data Acquisition & Control (Laura Newburgh, Nathan Whitehorn) [[File:S4_DAQ.pdf]] <br /><br />
'''15:00''' Data Management (Matthew Hasselfield) [[File:Data_management_20180906_v1.pdf]] <br /><br />
'''15:15''' Integration & Commissioning (Kam Arnold, Bradford Benson) [[File:IntegrationCommissioningPrinceton2018.pdf]] <br /><br />
'''15:30''' Options (Steve Padin) [[File:OptionsPrincetonV1.pdf]] <br /><br />
'''15:45''' Q&A<br />
<br />
'''16:00''' Fireslides 1 [[File:FireSlides_Thursday_post.pdf]]<br />
<br />
'''16:30''' Poster Session, Cocktails & Light Dinner<br />
<br />
------<br />
<br />
=== Friday September 7th ===<br />
<br />
'''08:00''' ''Breakfast''<br />
<br />
'''The CMB Circa September 2018'''<br />
<br />
'''08:30''' Harmonic Overtones (Marc Kamionkowski) [[File:Morningmarc.pdf]] <br /><br />
'''08:55''' On-sky performance of the CLASS Q-band telescope (John Appel) [[File:CLASS_S4_20180907_final.pdf]]<br /><br />
'''09:05''' SPIDER: an update, with foregrounds. Lots of them. (Bill Jones) <br /><br />
'''09:15''' Current state of the BICEP/Keck instrument, data and analysis (Clem Pryke) [[File:BK2018.pdf]] <br /><br />
'''09:25''' Planck 2018 and setting the stage for Stage-4 (Marius Millea) [[File:Planck2018.pdf]] <br /><br />
'''09:35''' Ground, Balloon, Space Complementarity (Shaul Hanany) [[File:PrincetonS4_2018V2.pdf]] <br /><br />
'''09:50''' BK-SPT3G forward plans (John Kovac) [[File:BK-SPT3G_forward.pdf]] <br /><br />
'''10:05''' Simons Observatory forward plans (Jo Dunkley) [[File:SO_plans.pdf]] <br /><br />
'''10:20''' The Big Step Up to CMB-S4 (Gil Holder) [[File:S4_Princeton_holder.pdf]] <br />
<br />
'''10:35''' ''Coffee Break''<br />
<br />
'''Adjacent Science & Emerging Ideas'''<br />
<br />
'''11:15''' Millimeter/Submillimeter Large Telescopes and Instruments (Phil Mauskopf) [[File:Mauskopf_princeton_cmbs4.pdf]]<br /><br />
'''11:30''' Intensity mapping meets the CMB: Complementary Cosmology across the radio spectrum (Laura Newburgh) [[File:2018_09_S4_IntensityMappingCMB.pdf]] <br /><br />
'''11:45''' SPHERE-X (Jamie Bock) [[File:Spherex_cmbs4_2018.pdf]] <br /><br />
'''12:00''' Weak Lensing (Elisabeth Krause) [[https://cmb-s4.org/wiki/images/Krause_LSSTxS4_2018.pdf slides_here]]<br />
<br />
'''12:15''' '' Group Photo & Lunch''<br />
<br />
'''13:15''' Reionization Studies in the CMB-S4 Era (Adam Lidz) <br /><br />
'''13:30''' A biased view of open questions in galaxy formation (Norm Murray) <br /><br />
'''13:45''' Polarized dust foreground models from HI data (Susan Clark) [[File:Clark_S4_ForegroundModels.pdf]] <br /><br />
'''14:00''' Properties of the magnetized dusty interstellar medium with Planck (Jonathan Aumont)<br />
<br />
'''Talks From Collaboration Members'''<br />
<br />
'''14:15''' Inflationary vs. Reionization Features from Current and Future Data (Cora Dvorkin) <br /><br />
'''14:25''' Stress-testing nonstandard neutrino physics with CMB-S4 (Francis-Yan Cyr-Racine) <br /><br />
'''14:35''' Searching for Dark Matter Interactions in the CMB (Kimberly Boddy) <br /><br />
'''14:45''' Foreground immune CMB lensing with shear-only reconstruction (Emmanuel Schaan) [[https://cmb-s4.org/wiki/images/Cmb_shear_schaan.pdf slides]]<br /><br />
'''14:55''' Cosmology from cross correlating S4 lensing with photometric galaxy counts (Blake Sherwin) [[File:NeutrinoXCorrs.pdf]] <br /><br />
'''15:05''' Higher order corrections to CMB lensing cross correlations (Vanessa Boehm) <br /><br />
'''15:15''' CMB lensing on small scales (Simone Ferraro) <br /><br />
'''15:25''' kSZ cosmology without the optical depth degeneracy (Mathew Madhavacheril) <br /><br />
'''15:35''' Q&A<br />
<br />
'''15:50''' ''Coffee Break''<br />
<br />
'''16:05''' Fireslides 2<br />
<br />
'''16:30''' Wrap-Up Panel - Roger Blandford, Chris Carilli, Bonnie Fleming, George Fuller, Risa Wechsler, Matias Zaldarriaga<br /><br />
Contributed material for panel discussion by panelists and audience:<br /><br />
*From George Fuller: [[File:Fuller-CMB-S4-Princeton.pdf]]<br /><br />
<br />
'''17:45''' Next Steps & Action Items<br />
<br />
'''Parallel Afternoon Session for Project Team'''<br />
<br />
'''15:00''' Charge for Decadal Survey Report Review on 12/11-13 in DC <br /><br />
'''15:30''' Possible DSR Review Committee and Planning Details <br /><br />
'''16:00''' Review of Overall Timeline and Boundary Conditions <br /><br />
'''16:30''' Critical Issues Identified in Project Planning <br /><br />
'''17:00''' Preparations/Guidance for Saturday Sessions <br /><br />
<br />
------<br />
<br />
=== Saturday September 8th ===<br />
<br />
'''08:30''' ''Breakfast''<br />
<br />
'''09:00''' Parallel Sessions<br />
* Science Council:<br />
** Noise & Forecasting (60 min)<br />
** White Paper Organization (45 min)<br />
* Technical Council:<br />
** Project Planning<br />
<br />
'''10:45''' ''Coffee Break''<br />
<br />
'''11:15''' Parallel Sessions<br />
*Science Council<br />
** AWG Working Meetings<br />
* Technical Council<br />
** Project Planning (continued)<br />
<br />
'''12:45''' ''Lunch (on your own)''<br />
<br />
'''13:45 onwards''' Rooms available for breakout sessions as required</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cmb_shear_schaan.pdf&diff=7524File:Cmb shear schaan.pdf2018-09-07T14:02:51Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Argonne-2018:P1-3&diff=6461Argonne-2018:P1-32018-03-06T06:12:37Z<p>Eschaan: /* Parallel session P1-3: Extending the Science case for the Decadal CDR (chair: Simone Ferraro) */</p>
<hr />
<div>Back to [[Argonne-2018: Cosmology with CMB-S4|Argonne 2018 main page]]<br />
<br />
== Parallel session P1-3: Extending the Science case for the Decadal CDR (chair: Simone Ferraro) ==<br />
<br />
*[[File:slides|Intro]]<br />
*[[:File:schaan_ksz.pdf|Emmanuel]]<br />
*[[File:slides|Elena]]<br />
*[[:File:Alvarez-eor.pdf|Marcelo]]<br />
*[[File:slides|Colin]]<br />
*[[File:slides|Rahul]]<br />
<br />
== Notes from session (Tuesday, March 6, 08:45-09:45) ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Argonne-2018:P1-3&diff=6460Argonne-2018:P1-32018-03-06T06:12:07Z<p>Eschaan: /* Parallel session P1-3: Extending the Science case for the Decadal CDR (chair: Simone Ferraro) */</p>
<hr />
<div>Back to [[Argonne-2018: Cosmology with CMB-S4|Argonne 2018 main page]]<br />
<br />
== Parallel session P1-3: Extending the Science case for the Decadal CDR (chair: Simone Ferraro) ==<br />
<br />
*[[File:slides|Intro]]<br />
*[[File:schaan_ksz.pdf|Emmanuel]]<br />
*[[File:slides|Elena]]<br />
*[[:File:Alvarez-eor.pdf|Marcelo]]<br />
*[[File:slides|Colin]]<br />
*[[File:slides|Rahul]]<br />
<br />
== Notes from session (Tuesday, March 6, 08:45-09:45) ==</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Schaan_ksz.pdf&diff=6459File:Schaan ksz.pdf2018-03-06T06:10:14Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2371Shear calibration LSST2016-05-24T16:33:47Z<p>Eschaan: </p>
<hr />
<div>(Emmanuel Schaan writing)<br />
Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST ([[File:zbins_LSST.pdf]]), while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.<br />
<br />
We consider different combinations of observables ([[File:Observables.pdf]]) and find the following 68% confidence constraints on the shear biases: [[File:LSST_summary_m.pdf]]. The main result is that the shear biases can be constrained to close to the LSST requirements, to about 0.5%. The method works best at higher z (where the correlation with CMB lensing is best), which is also where it is hardest to calibrate the shear otherwise. The calibration is robust to Gaussian photo-z errors and intrinsic alignments (not shown here).<br />
<br />
We assume that LSST and CMB S4 fully overlap on 18,000deg^2 (fsky=44%). The fiducial run assumes 1muK' and 1' for CMB S4, lmin=30 and lmax=3000 for T and 5000 for E and B. We show that the calibration is sensitive to the CMB S4 sensitivity [[File:LSST_varying_noise.pdf]] and not to the resolution [[File:LSST_varying_beam.pdf]]. This is mostly because of the fixed lmax imposed.</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=R_Forecasting_Logbook&diff=2193R Forecasting Logbook2016-05-18T18:13:41Z<p>Eschaan: </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 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 />
* 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 />
* 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 />
== Logbook Entries (reverse chronological) ==<br />
<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 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)</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=R_Forecasting_Logbook&diff=2192R Forecasting Logbook2016-05-18T18:12:52Z<p>Eschaan: </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 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 />
* 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 />
* 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 />
== Logbook Entries (reverse chronological) ==<br />
<br />
* '''2016 May 18''': [https://cosmo.uchicago.edu/CMB-S4workshops/index.php/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 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)</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=R_Forecasting_Logbook&diff=2191R Forecasting Logbook2016-05-18T18:12:29Z<p>Eschaan: </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 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 />
* 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 />
* 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 />
== Logbook Entries (reverse chronological) ==<br />
<br />
* '''2016 May 18''': [https://cosmo.uchicago.edu/CMB-S4workshops/index.php/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 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)</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2190Shear calibration LSST2016-05-18T18:10:30Z<p>Eschaan: </p>
<hr />
<div>(Emmanuel Schaan writing)<br />
Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST ([[File:zbins_LSST.pdf]]), while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.<br />
<br />
We consider different combinations of observables ([[File:Observables.pdf]]) and find that the following 68% confidence constraints on the shear biases: [[File:LSST_summary_m.pdf]]. The main result is that the shear biases can be constrained to close to the LSST requirements, to about 0.5%. The method works best at higher z (where the correlation with CMB lensing is best), which is also where it is hardest to calibrate the shear otherwise. The calibration is robust to Gaussian photo-z errors and intrinsic alignments (not shown here).<br />
<br />
We assume that LSST and CMB S4 fully overlap on 18,000deg^2 (fsky=44%). The fiducial run assumes 1muK' and 1' for CMB S4, lmin=30 and lmax=3000 for T and 5000 for E and B. We use the. We show that the calibration is sensitive to the CMB S4 sensitivity [[File:LSST_varying_noise.pdf]] and not to the resolution [[File:LSST_varying_beam.pdf]]. This is mostly because of the fixed lmax imposed.</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Forecasting&diff=2189Forecasting2016-05-18T18:08:34Z<p>Eschaan: </p>
<hr />
<div>===Forecasting non-r parameters===<br />
<br />
<br />
The expectation is that these forecasts will be done mainly using Fisher forecasts for the Science Book, with prudent use of frequencies and ell-range to avoid being over-optimistic about the impact of Galactic and extragalactic foregrounds and noise from the ground.<br />
<br />
----<br />
====Parameters ====<br />
Names of people responsible for generating forecasts in brackets. Sign yourself up and we can divide up tasks when we speak if there are multiple people.<br />
<br />
*LCDM 6-parameters (all)<br />
<br />
<br />
Inflation section<br />
*curvature (Stephen/Josquin) - also Danielle/Jo<br />
*running (Stephen/Josquin)<br />
*birefringence (Vera)<br />
*correlated isocurvature amplitude (Cora/Kimmy)<br />
*uncorrelated isocurvature amplitude (Cora/Kimmy)<br />
*compensated isocurvature ampltude (Julian/Ely)<br />
*axion isocurvature (Renee/Doddy/Dan)<br />
*cosmic string tension (Renee)<br />
*primordial magnetic field (TBD)<br />
<br />
<br />
Neutrino section<br />
*neutrino mass sum (Mat/Neelima/Nam) - also Alessandro<br />
*Neff (with delensing of TT & EE (Joel/Alex/Dan) - also Mat/Neelima/Nam and Erminia<br />
*Yp (with delensing of TT & EE (Joel/Alex/Dan) - also Erminia<br />
*neutrino sound speed (+Neff+mnu) [[File:S4_neutrinos.pdf]]-[[File:S4_neutrinos_fksy_lmin.pdf]] (Erminia)<br />
<br />
<br />
Dark matter and dark energy section<br />
*dark matter annihilation (Cora)<br />
*dark matter interactions (Cora)<br />
*utralight-axion density [[File:mass_m28_frac_sensitivity_resolution.pdf]] (Renee/Doddy/Dan G)<br />
*w (Alessandro) - also Stephen/Josquin<br />
*w0,wa (Alessandro) - also Stephen/Josquin<br />
*early dark energy (Erminia)<br />
*gamma (TBD)<br />
<br />
*kSZ S/N from S4 x photo-z (Simone)<br />
*[[Shear_calibration_LSST|shear bias calibration from S4 x LSST]] (Emmanuel)<br />
<br />
<br />
Here is place-holder for some suggested fiducial parameters and step-sizes, can be different though. Suggested new one: [[File:params_steps_v2.txt|500px]] (Original one here: [[File:params_steps.pdf|500px]])<br />
----<br />
<br />
====Fisher codes ====<br />
With info on what data they can handle and who is available to run them during next two months<br />
<br />
*Errard/Feeney code -unlensed TT, EE, TE and BB, plus deflection dd. Can do iterative EBEB, CIB or LSS delensing, and foreground removal on a statistical level. Current white noise, but simple to extend (Stephen,Josquin) -- web interface accessible at : http://portal.nersc.gov/project/mp107/index.html<br />
*Allison et al code - lensed TT/TE/EE plus kk plus BAO, can take in non-white N_ell but no explicit FG handling (Erminia Calabrese, Danielle Leonard, Jo Dunkley)<br />
*Extension of Allison et al code for axions (Renee Hlozek)<br />
*Stony Brook code - TT/TE/EE/kk with iterative delensing plus BAO, can take in non-white N_ell but no explicit FG handling, being expanded to include LSST shear and cluster counts with halo lensing (Mat Madhavacheril, Neelima Sehgal, Nam Nguyen)<br />
*de Bernardis code - includes kSZ likelihood (Francesco de Bernardis)<br />
*Manzotti code- similar to Allison et al and already partially checked against that code; used for http://arxiv.org/abs/1512.02654 (Alessandro Manzotti)<br />
*CITA code - includes delensing of spectra to all orders; forecasts of delensed covariances are in progress (Joel Meyers, Alex van Engelen, Dan Green)<br />
*who has a tSZ likelihood? (David Alonso can do N(M,z) and tSZ fluxes. Who has code to push through to parameters?)<br />
*other codes and people?<br />
<br />
<br />
----<br />
<br />
====Settings====<br />
<br />
Nominal:<br />
*S4 TT/TE/EE/kk over 40% of sky, 30<ell < lmax<br />
*Planck TT/TE/EE from 30<l<2500 over additional 20% of sky. Use these 'Planck-pol' specs for noise:[[File:planck_pol.pdf|500px]]<br />
*Planck TT at l<30 over 80% of sky<br />
*Tau prior 0.06+-0.01<br />
<br />
<br />
*lmax(TT)=3000 unless explicit foreground cleaning is done in code for kSZ etc<br />
*lmax(TE,EE)=5000 unless explicit foreground cleaning done in code<br />
*kk reconstructed from 30<l<lmax using MV estimate<br />
<br />
<br />
*quadratic estimator for lensing, ideally with iterative delensing<br />
*Gaussian likelihood neglecting T/E/k covariance is ok, but non-Gaussian better (do any codes have full lensed T/E/B/k covariance?)<br />
*non-linear power spectrum for kk, e.g. ok to use halofit in CAMB<br />
<br />
Extensions:<br />
*option to add DESI BAO. These are placeholder for forecast rs/DVs.[[File:bao_desi_v2.pdf|500px]]<br />
<br />
*cluster masses calibrated with LSST lensing or CMB halo lensing (need to refine what that means)<br />
<br />
----<br />
<br />
====Specs====<br />
<br />
''Nominal test case''<br />
*Single channel (e.g. 150 GHz) at 1 uK/amin in T and 1.4uK/amin in P, 3 arcmin resolution.<br />
*White noise, no FG inflation<br />
*Useful if your code can spit out errors as function of noise level in 1-10 uK/arcmin range and resolution in range 1-10 arcmin.<br />
<br />
''Next steps''<br />
<br />
*Define multiple frequencies of the survey<br />
*Decide if an N_ell that captures non-white-noise is necessary <br />
*Define residual FG level if any</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Forecasting&diff=2188Forecasting2016-05-18T18:07:03Z<p>Eschaan: </p>
<hr />
<div>===Forecasting non-r parameters===<br />
<br />
<br />
The expectation is that these forecasts will be done mainly using Fisher forecasts for the Science Book, with prudent use of frequencies and ell-range to avoid being over-optimistic about the impact of Galactic and extragalactic foregrounds and noise from the ground.<br />
<br />
----<br />
====Parameters ====<br />
Names of people responsible for generating forecasts in brackets. Sign yourself up and we can divide up tasks when we speak if there are multiple people.<br />
<br />
*LCDM 6-parameters (all)<br />
<br />
<br />
Inflation section<br />
*curvature (Stephen/Josquin) - also Danielle/Jo<br />
*running (Stephen/Josquin)<br />
*birefringence (Vera)<br />
*correlated isocurvature amplitude (Cora/Kimmy)<br />
*uncorrelated isocurvature amplitude (Cora/Kimmy)<br />
*compensated isocurvature ampltude (Julian/Ely)<br />
*axion isocurvature (Renee/Doddy/Dan)<br />
*cosmic string tension (Renee)<br />
*primordial magnetic field (TBD)<br />
<br />
<br />
Neutrino section<br />
*neutrino mass sum (Mat/Neelima/Nam) - also Alessandro<br />
*Neff (with delensing of TT & EE (Joel/Alex/Dan) - also Mat/Neelima/Nam and Erminia<br />
*Yp (with delensing of TT & EE (Joel/Alex/Dan) - also Erminia<br />
*neutrino sound speed (+Neff+mnu) [[File:S4_neutrinos.pdf]]-[[File:S4_neutrinos_fksy_lmin.pdf]] (Erminia)<br />
<br />
<br />
Dark matter and dark energy section<br />
*dark matter annihilation (Cora)<br />
*dark matter interactions (Cora)<br />
*utralight-axion density [[File:mass_m28_frac_sensitivity_resolution.pdf]] (Renee/Doddy/Dan G)<br />
*w (Alessandro) - also Stephen/Josquin<br />
*w0,wa (Alessandro) - also Stephen/Josquin<br />
*early dark energy (Erminia)<br />
*gamma (TBD)<br />
<br />
*kSZ S/N from S4 x photo-z (Simone)<br />
*[[ shear bias calibration from S4 x LSST]] (Emmanuel)<br />
<br />
<br />
Here is place-holder for some suggested fiducial parameters and step-sizes, can be different though. Suggested new one: [[File:params_steps_v2.txt|500px]] (Original one here: [[File:params_steps.pdf|500px]])<br />
----<br />
<br />
====Fisher codes ====<br />
With info on what data they can handle and who is available to run them during next two months<br />
<br />
*Errard/Feeney code -unlensed TT, EE, TE and BB, plus deflection dd. Can do iterative EBEB, CIB or LSS delensing, and foreground removal on a statistical level. Current white noise, but simple to extend (Stephen,Josquin) -- web interface accessible at : http://portal.nersc.gov/project/mp107/index.html<br />
*Allison et al code - lensed TT/TE/EE plus kk plus BAO, can take in non-white N_ell but no explicit FG handling (Erminia Calabrese, Danielle Leonard, Jo Dunkley)<br />
*Extension of Allison et al code for axions (Renee Hlozek)<br />
*Stony Brook code - TT/TE/EE/kk with iterative delensing plus BAO, can take in non-white N_ell but no explicit FG handling, being expanded to include LSST shear and cluster counts with halo lensing (Mat Madhavacheril, Neelima Sehgal, Nam Nguyen)<br />
*de Bernardis code - includes kSZ likelihood (Francesco de Bernardis)<br />
*Manzotti code- similar to Allison et al and already partially checked against that code; used for http://arxiv.org/abs/1512.02654 (Alessandro Manzotti)<br />
*CITA code - includes delensing of spectra to all orders; forecasts of delensed covariances are in progress (Joel Meyers, Alex van Engelen, Dan Green)<br />
*who has a tSZ likelihood? (David Alonso can do N(M,z) and tSZ fluxes. Who has code to push through to parameters?)<br />
*other codes and people?<br />
<br />
<br />
----<br />
<br />
====Settings====<br />
<br />
Nominal:<br />
*S4 TT/TE/EE/kk over 40% of sky, 30<ell < lmax<br />
*Planck TT/TE/EE from 30<l<2500 over additional 20% of sky. Use these 'Planck-pol' specs for noise:[[File:planck_pol.pdf|500px]]<br />
*Planck TT at l<30 over 80% of sky<br />
*Tau prior 0.06+-0.01<br />
<br />
<br />
*lmax(TT)=3000 unless explicit foreground cleaning is done in code for kSZ etc<br />
*lmax(TE,EE)=5000 unless explicit foreground cleaning done in code<br />
*kk reconstructed from 30<l<lmax using MV estimate<br />
<br />
<br />
*quadratic estimator for lensing, ideally with iterative delensing<br />
*Gaussian likelihood neglecting T/E/k covariance is ok, but non-Gaussian better (do any codes have full lensed T/E/B/k covariance?)<br />
*non-linear power spectrum for kk, e.g. ok to use halofit in CAMB<br />
<br />
Extensions:<br />
*option to add DESI BAO. These are placeholder for forecast rs/DVs.[[File:bao_desi_v2.pdf|500px]]<br />
<br />
*cluster masses calibrated with LSST lensing or CMB halo lensing (need to refine what that means)<br />
<br />
----<br />
<br />
====Specs====<br />
<br />
''Nominal test case''<br />
*Single channel (e.g. 150 GHz) at 1 uK/amin in T and 1.4uK/amin in P, 3 arcmin resolution.<br />
*White noise, no FG inflation<br />
*Useful if your code can spit out errors as function of noise level in 1-10 uK/arcmin range and resolution in range 1-10 arcmin.<br />
<br />
''Next steps''<br />
<br />
*Define multiple frequencies of the survey<br />
*Decide if an N_ell that captures non-white-noise is necessary <br />
*Define residual FG level if any</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2187Shear calibration LSST2016-05-18T18:04:05Z<p>Eschaan: </p>
<hr />
<div>Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST ([[File:zbins_LSST.pdf]]), while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.<br />
<br />
We consider different combinations of observables ([[File:Observables.pdf]]) and find that the following 68% confidence constraints on the shear biases: [[File:LSST_summary_m.pdf]]. The main result is that the shear biases can be constrained to close to the LSST requirements, to about 0.5%. The method works best at higher z (where the correlation with CMB lensing is best), which is also where it is hardest to calibrate the shear otherwise. The calibration is robust to Gaussian photo-z errors and intrinsic alignments (not shown here).<br />
<br />
We assume that LSST and CMB S4 fully overlap on 18,000deg^2 (fsky=44%). The fiducial run assumes 1muK' and 1' for CMB S4, lmin=30 and lmax=3000 for T and 5000 for E and B. We use the. We show that the calibration is sensitive to the CMB S4 sensitivity [[File:LSST_varying_noise.pdf]] and not to the resolution [[File:LSST_varying_beam.pdf]]. This is mostly because of the fixed lmax imposed.</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:LSST_varying_beam.pdf&diff=2186File:LSST varying beam.pdf2016-05-18T17:55:00Z<p>Eschaan: </p>
<hr />
<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:LSST_varying_noise.pdf&diff=2185File:LSST varying noise.pdf2016-05-18T17:54:30Z<p>Eschaan: </p>
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<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:LSST_summary_m.pdf&diff=2184File:LSST summary m.pdf2016-05-18T17:51:53Z<p>Eschaan: </p>
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<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Observables.pdf&diff=2183File:Observables.pdf2016-05-18T17:50:23Z<p>Eschaan: </p>
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<div></div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2182Shear calibration LSST2016-05-18T17:48:17Z<p>Eschaan: </p>
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<div>Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST ([[File:zbins_LSST.pdf]]), while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2181Shear calibration LSST2016-05-18T17:47:17Z<p>Eschaan: </p>
<hr />
<div>Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST, while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.<br />
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<br />
<pdf>File:zbins_LSST.pdf</pdf> <br />
<br />
<pdf width="500" height="300">File:zbins_LSST.pdf</pdf><br />
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[[File:zbins_LSST.pdf|page=1]]</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2180Shear calibration LSST2016-05-18T17:46:47Z<p>Eschaan: </p>
<hr />
<div>Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST, while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.<br />
<br />
<br />
<pdf>File:zbins_LSST.pdf</pdf> <br />
<br />
[[File:zbins_LSST.pdf|page=1]]</div>Eschaanhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Shear_calibration_LSST&diff=2179Shear calibration LSST2016-05-18T17:46:17Z<p>Eschaan: </p>
<hr />
<div>Here are some preliminary forecasts for calibrating the shear bias from LSST using CMB lensing from CMB S4 (paper in preparation with Tim Eifler, Elisabeth Krause, Hironao Miyatake, Olivier Doré, Jason Rhodes and David Spergel). We use all the 2-point correlations of galaxy positions, convergence from galaxies and convergence from the CMB. In particular, we use only the convergence from CMB S4 (e.g. not the temperature and polarization power spectrum). We constrain 10 shear biases for each of the 10 source redshift bins of LSST, while marginalizing over cosmological parameters, galaxy biases, and photo-z means and variances in each bin. We use the full non-Gaussian covariances for all the 2-point functions, and explore the likelihood with MCMC.<br />
<br />
<br />
<pdf>zbins_LSST.pdf</pdf> <br />
<br />
[[File:zbins_LSST.pdf|page=1]]</div>Eschaan