UMICH-2015: Inflation break-out session 1

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B-modes challenges: foregrounds and de-lensing

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Foregrounds

  • What are our latest estimates of foreground levels post-Planck?
  • What simulations and tools do we have for forecasting impact on r?
  • What are still physical unknowns?
  • Do we need new data at <40 GHz and >230 GHz?
  • How important is large sky area?

Delensing

  • What is the impact of delensing on r, and on nt?
  • How does internal CMB delensing compare to external (e.g. CIB)?
  • What sensitivity and resolution do we need for the lensing map?
  • How important is it to have lensing map from the same instrument?


Foregrounds

  • What are our latest estimates of foreground levels post-Planck? (Steve, Raphael...)

Can we make a new version of this figure:

OldFG.png


  • What simulations and tools do we have for forecasting impact on r? (Jacques, Raphael, Stephen F, Aurelien, Jo)

Is there a new PSM? Common sim maps would be great.


  • What are still physical unknowns? (Al Kogut?)

Magnetic dust, spinning dust polarization, spatial dispersion of dust temperature/emissivity...


  • Do we need new data at <40 GHz and >230 GHz? (Jo)

  • How important is large sky area?

Delensing

(Blake Sherwin, Olivier Dore, Chris Sheehy, Josquin Errard, Stephen Feeney, Alex van Engelen, Neelima Sehgal...)

  • What is the impact of delensing on r, and on nt?

  • How does internal CMB delensing compare to external (e.g. CIB)?

Blake says external cleaning won't be good enough for 1 uK noise levels.


  • What sensitivity and resolution do we need for the lensing map?

  • How important is it to have lensing map from the same instrument?