# Difference between revisions of "UCSD-2019: Cross-Cut: Simulations for Measurement Requirements"

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* 5 min - Marcelo Alvarez: Extragalactic modeling integration in PySM 3, Simulations requirements for cluster finding [[File:exgal_sims.pdf]] | * 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 [https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II Chile deep] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile Chile wide] [https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole Pole deep] [https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II Pole wide] | * 5 min - Reijo Keskitalo: Scanning strategy for S4 [https://cmb-s4.org/wiki/index.php/Deeper_SAT_from_Chile_II Chile deep] [https://cmb-s4.org/wiki/index.php/High_cadence_LAT_from_Chile Chile wide] [https://cmb-s4.org/wiki/index.php/Deep_SAT_from_the_Pole Pole deep] [https://cmb-s4.org/wiki/index.php/Wider_SAT_from_the_Pole_II Pole wide] | ||

− | * 5 min - Ben Racine: Noise simulations for PGW analysis [[File:noise_sims_for_forecasting.pdf]] | + | * 5 min - Ben Racine: Noise simulations for PGW analysis [[:File:noise_sims_for_forecasting.pdf|Sims for PGW]] |

* 30 min - Discussion: | * 30 min - Discussion: | ||

** Unified sky model | ** Unified sky model | ||

Line 30: | Line 30: | ||

[https://hackmd.io/o1KtRAHXSliAP-sfL73r8A Collaborative note taking on hackMD] | [https://hackmd.io/o1KtRAHXSliAP-sfL73r8A Collaborative note taking on hackMD] | ||

+ | |||

+ | = Cross-Cut: Simulations for Measurement Requirements = | ||

+ | |||

+ | [https://cmb-s4.org/wiki/index.php/UCSD-2019:_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 (<code>so_pysm_models</code>) 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 ==== | ||

+ | |||

+ | * 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: 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?? |

## Latest revision as of 13:14, 19 October 2019

## Contents

## 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

## Notes

Collaborative note taking on hackMD

# Cross-Cut: Simulations for Measurement Requirements

## 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

- 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

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??