UCSD-2019: Analysis/Pipeline Working Group: Sources
Charge
Given plausible CIB models (and galactic foregrounds) at high ell, what frequency coverage (and associated sensitivity) is sufficient to meet our goals for z> 2 clusters?
What are the benefits to time-domain science of increased ang. Resolution and increased sensitivity?
What are the necessary analysis tools to answer these questions?
Agenda
George Stein (Webskys) (15min) File:Websky Oct2019.pdf
Joaquin Vieira (Source Counts) (15min) File:CMB-S4 point sources vieira Oct2019.pdf
Srini Raghunathan (15min) (Cluster detection, presented by Gil Holder) File:SRaghunathan GHolder sources.pdf
Gil Holder (Asteroids) (15min) slides
Discussion: (60 min) what do we need going forward?
== Remote Attendance
Zoom link (don't use)
Zoom link (use this one !)
