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

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(Charge)
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== Charge ==
 
== Charge ==
  
 
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* 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?
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* 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 ==
 
== Agenda ==

Revision as of 13:40, 11 October 2019

Link back to agenda

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

Remote attendance

Zoom link


Notes