# Difference between revisions of "UCSD-2019: Analysis/Pipeline Working Group: Maps to Other Statistics"

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== Agenda == | == Agenda == | ||

+ | |||

+ | * Lensing | ||

+ | |||

+ | Foregrounds: | ||

+ | |||

+ | Emmanuel Schaan: temperature foregrounds in lensing (20+10 mins) | ||

+ | Kevin Huffenberger: modeling of small-scale non-Gaussian foregrounds (to characterize lensing bias) (10+5 mins) | ||

+ | Srini Raghunathan: foregrounds for cluster lensing reconstruction (10+5 mins) | ||

+ | |||

+ | Theory: | ||

+ | |||

+ | Alex van Engelen: baryonic effects for CMB lensing and neutrino mass (10+5 mins) | ||

+ | |||

+ | * kSZ | ||

== Remote attendance == | == Remote attendance == |

## Revision as of 13:37, 13 October 2019

## Contents

## Charge

- Given plausible CIB models (and galactic foregrounds) at high ell, what frequency coverage (and associated sensitivity) is sufficient to reduce CIB residuals below statistical errors on tSZ and kSZ measurements?
- How severe is the impact of small-scale polarized foregrounds on lensing? (If important, how can we mitigate them?)
- What is the optimal strategy for mitigating temperature lensing foregrounds?
- What are requirements on beam and pointing for sub-percent lensing spectra?
- What are the necessary analysis tools to answer these questions?

## Agenda

- Lensing

Foregrounds:

Emmanuel Schaan: temperature foregrounds in lensing (20+10 mins) Kevin Huffenberger: modeling of small-scale non-Gaussian foregrounds (to characterize lensing bias) (10+5 mins) Srini Raghunathan: foregrounds for cluster lensing reconstruction (10+5 mins)

Theory:

Alex van Engelen: baryonic effects for CMB lensing and neutrino mass (10+5 mins)

- kSZ

## Remote attendance