UCSD-2019: Cross-Cut: Simulations for Measurement Requirements

Link back to agenda

Charge

• How do we coordinate the production of a unified sky model with enough realism and flexibility for the AWGs?
• What simulations do we need for clusters and what cross-checks will be available with data?

Agenda

Please add your name below the agenda if you plan to participate in the session, contact User:Zonca

• 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory
• 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding File:Exgal sims.pdf
• 5 min - Reijo Keskitalo: Scanning strategy for S4 Chile deep Chile wide Pole deep Pole wide
• 5 min - Ben Racine: Noise simulations for PGW analysis Sims for PGW
• 30 min - Discussion:
  • Unified sky model
  • How to gather requirements from AWG
  • Clusters
  • Plans for map-based simulations

Other participants: Raphael Flauger, Kimmy Wu

Remote attendance

Zoom link

Notes

Collaborative note taking on hackMD

Cross-Cut: Simulations for Measurement Requirements

Link to wiki

Agenda and notes

• 5 min - Andrea Zonca: PySM 3, simulation tools developed for Simons Observatory
• 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding
• 5 min - Reijo Keskitalo: Scanning strategy for S4
• 5 min - Ben Racine: Noise simulations for PGW analysis
• 25 min - Discussion:

Unified sky model

Galactic

• PySM (so_pysm_models) NSIDE 8192 Planck + Gaussian
• MHD: Dust + Synch small patches
• d7 - implement in PySM 3 and increase resolution
• Currently used model up until DSR by the r-forecasting group:
  • 00 - Simple Gaussian Sync/Dust with uniform amplitude across the sky
  • 01 - PySM base (@zonca has higher nside than 512, to 4096? will get to 8192)
  • 02 - PySM extended (@zonca has higher nside than 512, to 4096? will get to 8192)
  • 03 - Same as 02 but Hensley/Draine dust model
  • 04 - HiDPol dust model (by Tuhin Ghosh)
  • 05 - Strong decorrelation model
  • 06 - MHD based model from Flauger/Hensley (should swap in "08": one with more correct synchrotron)
  • 07 - Amplitude modulated Gaussian
  • 08 - MKD multilayer model from arxiv/1706.04162
  • 09 - Vansyngel model as described in arxiv/1611.02577 with multi-frequency extension
• For delensing, we need small scale polarized non-Gaussian Galactic foregrounds. Currently, only 09 has small scale NG.
• discuss: 00 should be replaced with 07? 00 won't be meaningfully used by the large area survey. But it is useful for the deep survey for sanity checks.
• To generalize 08 and 09 into PySM, @zonca has to ask the creator of these models for code/info.
• Q: are there other Galactic models used in S4 outside of the r-forecasting group?
• Check consistency with Planck
• CO lines?

Extragalactic + Clusters

• Websky, 1 realization
• validated against planck
• lensing: 1 realization
• radio galaxy sources, catalog input, PySM component could generate map on the fly
• tSZ from Planck, CIB from Herschel and Planck, dusty galaxy count compared to Herschel, stack clusters

Noise

Scanning strategy

• https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II
• https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile

High cadence LAT gives lot of f_sky and daily scans for transients

• https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole

Below only done in case of r detection from Deep SAT:

• https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II

Jan & Feb we could remove

Clem has already noise pipeline

Delensing LAT from Pole??

Noise simulations for PWG

• SAT BK start from data, fit noise model, just scaling NET, Pole
• BK noise calculator does not agree with data
• Noise calculator is just used for LAT
• Extrapolating 220 to 270, same below
• Check POLARBEAR new released performance, use that to scale?

Delensing LAT at Pole needs a noise model, maybe scaling SPT??