Difference between revisions of "UMICH-2015: Inflation break-out session 1"
| Line 42: | Line 42: | ||
Magnetic dust, spinning dust polarization, spatial dispersion of dust temperature/emissivity... | 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 GHz? (Jo) | + | *Do we need new data at <40 GHz and >230 GHz? (Clem/John?, Jo) |
| + | |||
| + | The effective polarized noise from cleaning a 150 GHz map with the Planck 353 GHz data is about 19 uK-arcmin, i.e. an additional uncertainty on r of ~0.01 for a survey covering 20% of the sky | ||
| + | |||
| + | [[File:index.png|500px]] | ||
----- | ----- | ||
Revision as of 16:25, 17 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?
- 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:
- 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...
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 GHz? (Clem/John?, Jo)
The effective polarized noise from cleaning a 150 GHz map with the Planck 353 GHz data is about 19 uK-arcmin, i.e. an additional uncertainty on r of ~0.01 for a survey covering 20% of the sky
- 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?
