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

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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?

How to gather requirements from AWG

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

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

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

Jan & Feb we could remove

Clem has already noise pipeline

Delensing LAT from Pole??

Noise simulations for PWG

  • SAT: start from BK data, fit noise model, just scaling NET and observing time, only data from Pole
  • BK NET calculator does not agree with data (in absolute terms), but only relative scaling matters
  • Noise calculator is just used for LAT
  • SAT: Extrapolating 220 to 270, 95GHz to lower freqs. Will need to be checked when data is available.
  • Check POLARBEAR new released performance, use that to scale?

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