Difference between revisions of "Sources Project List"

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If you are interested in any of the project shown below please email Joaquin and Nick to discuss how you can contribute.  
 
If you are interested in any of the project shown below please email Joaquin and Nick to discuss how you can contribute.  
  
==Clusters==
+
=Clusters=
 
This project will focus on tightening up the science to measurements flow-down for clusters:
 
This project will focus on tightening up the science to measurements flow-down for clusters:
* Set up a series of map-based simulations of the exaSimulate galactic sky that includs clusters
+
* Set up a series of map-based simulations of the extragalactic sky (which includes SZ clusters).
 
* Obtain sky/experimental noise maps for the given frequency channels and include realistic scanning strategies. Here we will perturb the frequency bands, resolution and depth.
 
* Obtain sky/experimental noise maps for the given frequency channels and include realistic scanning strategies. Here we will perturb the frequency bands, resolution and depth.
 
* Run cluster finders (SPT and ACT) on simulated maps (+noise)
 
* Run cluster finders (SPT and ACT) on simulated maps (+noise)
 
* Assess the feasibility to obtain science goals given experimental configuration.  
 
* Assess the feasibility to obtain science goals given experimental configuration.  
=Lower priority=
+
==Lower priority==
 
* Run CMB lensing estimators on these same maps (synergy here with Maps2Other).
 
* Run CMB lensing estimators on these same maps (synergy here with Maps2Other).
  
  
==Transients==
+
=Transients=
 
This project will focus on tightening up the science to measurements flow-down for transients:
 
This project will focus on tightening up the science to measurements flow-down for transients:
 
* Pin down how fast the alert needs to be generated from when the observation has finished. In principle, this could be done an hour after each observation takes place. This would mean there would be alerts going out ~3 times per day, roughly an hour after the observation is finished
 
* Pin down how fast the alert needs to be generated from when the observation has finished. In principle, this could be done an hour after each observation takes place. This would mean there would be alerts going out ~3 times per day, roughly an hour after the observation is finished
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* Compare the differences between Pole and Chile observing+map making for processing speed etc.
 
* Compare the differences between Pole and Chile observing+map making for processing speed etc.
  
==Point Sources==
+
=Point Sources=
 
The main thrust of point source work will focus on "proto-clusters" as blazars, SMGs, and lensed sources are all well characterized:
 
The main thrust of point source work will focus on "proto-clusters" as blazars, SMGs, and lensed sources are all well characterized:
 
* A big uncertainty is the density and luminosity of “proto-clusters”. Here we can extrapolate from SPT counts (~5 sources) and compare to models (which naively imply ~1e5 protoclusters for S4).
 
* A big uncertainty is the density and luminosity of “proto-clusters”. Here we can extrapolate from SPT counts (~5 sources) and compare to models (which naively imply ~1e5 protoclusters for S4).
 
* Find ways to connect (models, observations, and science case) the SZ cluster population (mm decrement) to the higher z and lower mass proto-clusters (mm increment).
 
* Find ways to connect (models, observations, and science case) the SZ cluster population (mm decrement) to the higher z and lower mass proto-clusters (mm increment).

Latest revision as of 20:13, 25 November 2019

If you are interested in any of the project shown below please email Joaquin and Nick to discuss how you can contribute.

Clusters

This project will focus on tightening up the science to measurements flow-down for clusters:

  • Set up a series of map-based simulations of the extragalactic sky (which includes SZ clusters).
  • Obtain sky/experimental noise maps for the given frequency channels and include realistic scanning strategies. Here we will perturb the frequency bands, resolution and depth.
  • Run cluster finders (SPT and ACT) on simulated maps (+noise)
  • Assess the feasibility to obtain science goals given experimental configuration.

Lower priority

  • Run CMB lensing estimators on these same maps (synergy here with Maps2Other).


Transients

This project will focus on tightening up the science to measurements flow-down for transients:

  • Pin down how fast the alert needs to be generated from when the observation has finished. In principle, this could be done an hour after each observation takes place. This would mean there would be alerts going out ~3 times per day, roughly an hour after the observation is finished
  • Refine rate estimates and pin down the requirement for the promptness of the alert generation (In contact with Berger and Meztger).
  • Interface with the scan strategy group and fold in the time variability of on-axis GRBs in the mm, a few hours after observation should be fine for both the science and the logistics.
  • Compare the differences between Pole and Chile observing+map making for processing speed etc.

Point Sources

The main thrust of point source work will focus on "proto-clusters" as blazars, SMGs, and lensed sources are all well characterized:

  • A big uncertainty is the density and luminosity of “proto-clusters”. Here we can extrapolate from SPT counts (~5 sources) and compare to models (which naively imply ~1e5 protoclusters for S4).
  • Find ways to connect (models, observations, and science case) the SZ cluster population (mm decrement) to the higher z and lower mass proto-clusters (mm increment).