__Nov. 22 2017__

Attendees:

Agenda:

  Brief update on new specs for imager and PICO workshop (Shaul, Nick)

[[imageroptions|Imager Options]]

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)

{{::input_tsz.png?direct&80 |input tSZ map}}

{{::NILC_PICO_tsz.png?direct&80 |Component separated tSZ map}}

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)

{{::alvarez_reionisation_tau.pdf|Reionization slides}}

{{::reionization_contours_zbar_delz_pico.png?direct&100 |Reion Constraints}} 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 [[start:stm|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__