Difference between revisions of "UMICH-2015: Inflation break-out session 1"

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===Delensing===  
 
===Delensing===  
(Blake Sherwin, Olivier Dore, Chris Sheehy, Josquin Errard, Stephen Feeney, Alex van Engelen, Neelima Sehgal...)
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(Blake Sherwin, Olivier Dore, Chris Sheehy, Josquin Errard, Stephen Feeney, Alex van Engelen, Neelima Sehgal, Anthony Challinor...)
  
*What is the impact of delensing on r, and on nt?  
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*What is the impact of delensing on r, and on nt or BB wiggles?  
  
 
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Revision as of 06:41, 18 September 2015

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B-modes challenges: foregrounds and de-lensing

Return to main workshop page

Return to Inflation sessions page


Foregrounds

  • What are our latest estimates of foreground levels post-Planck?
  • What simulations and tools do we have for forecasting impact on r? (details for Tuesday)
  • 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 or BB wiggles?
  • How does internal CMB delensing compare to external (e.g. CIB)?
  • What sensitivity and resolution do we need for the lensing map?

Foregrounds

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

Figure from Steve Choi/Lyman Page:

Choi.png

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) - detailed discussion on Tuesday

Is there a new PSM? http://www.apc.univ-paris7.fr/~delabrou/PSM/psm.html. Common sim maps would be great. Ability to do quick and dirty forecasts always good for exploring different set-ups.


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

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

From Planck, dispersion in dust index between individual 300 deg2 patches is about +-0.15 and varies between beta = 1.1 and 2.2.


  • Do we need new data at <40 GHz and >230-300 GHz? (Clem/John?, Mark)

The effective polarized noise from cleaning 150 GHz with Planck 353 GHz is about 19 uK-arcmin, i.e. an additional sigma(r) ~0.01 for fsky=0.2

Index.png


  • How important is large sky area?

Delensing

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

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

  • 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?