Nov. 22 2017
Attendees:
Agenda:
Brief update on new specs for imager and PICO workshop (Shaul, Nick)
Use v2.7 under the heading Frequency Bands and Noise: Specifications to Use
The resolution is the same, there are more detectors → lower noise levels.
Pico conference in the spring 2018 (time still TBD), please let us know if you are interested in attedning and presenting something.
y-map and component separation (Mathieu)
Smoothed at 3' resolution. The NILC reconstruction looks pretty clean
Propagate the NILC weights to the individual foreground components and compute the angular power spectra to give a picture of the residual foreground contamination in the NILC y-map.
Produce an SZ-free CMB map using the “Constrained ILC” method (Remazeilles et al 2011), which might be useful for kinetic SZ and/or cross-correlation with LSS surveys.
Reionization (Marcelo & Renee)
Work with Marcelo and Renee to sync up models with the constraints for this illustration
Explore other parameters
Refine contours
STM update (Nick)
The STM is here Science Traceability Matrix
Legacy Catalogs
| Catalog | Impact | Science |
| proto-clusters | Thousands of proto-clusters selected homogeneously, compared to heterogeneous samples of a few | galaxy cluster formation, early ICM properties, … |
|---|---|---|
| Lensed Point sources | 3,000 rare highly magnified dusty sources compared to ~10s sources found by Planck | sub-structure, high-z star formation,… |
| High-z galaxy clusters | ~ 100s of virialized clusters and z >~ 2 | galaxy formation in dense environments at the peak of star formation for most cluster galaxies, ICM,… |
| Polarized Point Sources | Direct counts in polarization both for radio sources and for dusty galaxies (1st time) |
AOB
Minutes