sept._20_2017 [Probe Mission Study Wiki]

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Sept. 20th 2017

Attendees: Alex, Lindsey, Jean-Baptiste, Shaul, Gianfranco, Max, Colin, Jacques
Apologies: Jim

Agenda:

Nick - Working group overview, goals, and logistics
Identify the primary Extragalactic science targets for the Probe, and how these science targets are affected by the Probe’s design 
Science targets include: Reionization, Galaxy formation at z > 2,  Thermodynamics of Galaxy formation, Clusters, and Lensing, add your additional target here
Address what are the science drivers for frequency higher than 460 GHz band
STM

Should we make Wednesday 10am our nominal call time? Shaul has arranged for a continuing webex meeting at this time
How do we want to and what the most effective way to share results? wiki? Google docs?
Important dates Sept 27th and Oct 25th the EC would like a summary from our group.

Gianfranco - Point Source Science 
SEE Gianfranco’s post

Jacques - CORE simulations, availability, and portability to the Probe 

Lindsey - Argonne simulation effort
Tabled to next week

Jim & Jean-Baptiste - CORE cluster science overview and portability to the Probe 
Nick - Clusters
Nick - Some interesting cluster neutrino mass constraints:
  * S4-max + Optical lensing calibration: ~ 25 meV (Planck tau)
  * CMB Probe + Optical lensing calibration: ~ 20 meV (CMB Probe tau)
  * S4-max + Optical lensing calibration: ~ 10 meV (CMB Probe tau)

Alex - Lensing S/N estimates
  * http://www.cita.utoronto.ca/~engelen/plots/cmbprobe_noisecurves.pdf - The noise curves for Cmbprobe which Nick sent me, together with the minimum-variance combination that I get when I just coadd them all without regard to the existence of any foreground power (or any non-CMB signals)  (thick black).  The result has a temperature noise of 0.8 uK-arcmin.
  *
  * http://www.cita.utoronto.ca/~engelen/plots/cmbprobe_lensingnoise.pdf - Lensing noise curves for Cmbprobe (red) and CMB-S4 (blue).  Note CMB-S4 has slightly higher noise but much better angular resolution.  I set lmax = 5000 for both TT and pol (although usually we set it to 3000 for TT) and I assumed f_sky = 0.4.  The EB curves include the impact of iterative delensing for both experiments.

Colin & Max & Nick - Component separation / y-maps
Table for next week
	
Nick - Reionization

We know very little about Reionization. The CMB Probe will delivery CV tau measurements, what does that mean for Reionization models? Given that we have high resolution measurements from the ground delivering kSZ power spectrum measurements and high order statistics (e.g. Smith & Ferraro 2017) CV will constrain.

Here I’ve combined AdvACT-like kSZ constraints with a CV tau constraint from CMB Probe in the mean reionization redshift and duration of reionization plane. The blue 1 & 2 sigma contours show show the what the addition of the Probe constraints provide compared to the Planck (orange contours).
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