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?

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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:

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• 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.

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• 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.

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• 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

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• How important is large sky area?

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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?

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• 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.

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

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