Minutes from Sept 13 2017

Attendees: Sebastian, Jean-Baptiste, Colin, Nick

Introduction to the WG goals

-Provide science cases for the CMB Probe -Inform the Executive Committee on the trade-off between science and design -Provide input into the STM

We have been tasked to provide the science areas to EC where CMB-probe will be transformative (or close to it). These topics are not fixed, but here are the initial topics:

-Galaxy formation at z > 2 -Reionization -Galaxy Formation Thermodynamics

Additional topics where CMB probe could have potentially interesting results:

-Clusters -CMB Lensing

Is the experiment design fix?

No there’s a chance to modify the design, so we should perturb around the spread sheet that’s been posted, in resolution, sensitivity, and frequency channels.

Are there sims?

Not at the moment, hopefully LBL and Argonne will provide something in the near future, they have been mostly focused on S3 and S4 ground based experiments. There are simulations for CORE, that we could be possibly use in the meantime. Please ask Jacques about the CORE simulations.

Outline of our procedure for filling out the STM -develop a paragraph or two for each science case, outline the importance how CMB probe adds to it -produce figures to accompany the above text -perturb about the fiducial CMB probe design -distill the above text and figures into the STM

-Upcoming important deadlines Sept. 27 report to EC Oct. 25 report to EC

Posts: Point Sources (Gianfranco)

Clusters (Nick)

Cluster numbers for the probe with and without 555 GHz and greater. Note: fsky for these forecast was 0.7

With 555 GHz and above:

Full CMB probe w/ LSST WL mass calibration + Planck tau: # clusters ~27200

Mnu 1-sigma : 29.3 meV

w0 1-sigma : 5.08 %

wa 1-sigma : 0.25

Only up to (and excluding?) 555 GHz

Full CMB probe w/ LSST WL mass calibration + Planck tau

# clusters ~24600

Mnu 1-sigma : 30.0 meV

w0 1-sigma : 5.35 %

wa 1-sigma : 0.26

Please note that the foregrounds in these forecasts are stochastic and not correlated, so to see the real impact of the these higher frequencies we need to include correlated foregrounds. Furthermore we can update the tau constraints to include CMB-Probe estimates which should be close to CV limited.

Other Business: None