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--- nov._22_2017 [2017/11/22 08:43] – nbatta
+++ nov._22_2017 [2017/11/22 09:15] (current) – nbatta
@@ Line 5: / Line 5: @@
 Agenda:
-  Brief update on new specs for imager (Shaul, Nick)
+  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)
@@ Line 21: / Line 39: @@
   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__

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