Difference between revisions of "UMICH-2015: Inflation break-out session 1"
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*Do we need new data at <40 GHz and >230 GHz? (and 60 GHz?) | *Do we need new data at <40 GHz and >230 GHz? (and 60 GHz?) | ||
*How important is large sky area? | *How important is large sky area? | ||
| + | *What is the path to a convincing claim that a B-mode signal is not foregrounds? | ||
===Delensing=== | ===Delensing=== | ||
Revision as of 08:01, 20 September 2015
B-modes challenges: foregrounds and de-lensing
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? (and 60 GHz?)
- How important is large sky area?
- What is the path to a convincing claim that a B-mode signal is not foregrounds?
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:
Can we make a new version of this figure:
- 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
- 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?
