Difference between revisions of "UMICH-2015: Inflation break-out session 2"

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(Created page with "==Wiki navigation== Return to main workshop page Return to Inflation sessions page")
 
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[[UMICH-2015: Inflation|Return to Inflation sessions page]]
 
[[UMICH-2015: Inflation|Return to Inflation sessions page]]
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==Spectral Index, Running, Non-Gaussianity, ...==
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1. For which observables do we have well-motivated theory thresholds?
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  - r: One may argue there are two interesting thresholds, r~0.01 and r~0.003.
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  - nt: slow-roll consistency condition.
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  - running: The value predicted by slow-roll inflation is a well-defined target.
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  - non-Gaussianity: There are various thresholds, local fNL=1, equilateral fNL=1, slow-roll fNL
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  - curvature: \Omega_K~0.0001.
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  - Is there a threshold for ns, contributions from isocurvature modes, features, other inflationary observables?
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2. Can we reach these thresholds in an ideal experiment, and if so can we reach them with CMB S4?
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  - Is there hope to measure the largest angular scales from the ground?
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  - How far can we go in multipole space in polarization, i.e. how well do we understand polarized foregrounds
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    from small scale experiments?
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3. Given the focus on inflation, neutrinos and dark energy, are we missing interesting observables/opportunities?
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  -e.g. constraints on primordial magnetic fields

Revision as of 16:25, 16 September 2015

Wiki navigation

Return to main workshop page

Return to Inflation sessions page

Spectral Index, Running, Non-Gaussianity, ...

1. For which observables do we have well-motivated theory thresholds?

 - r: One may argue there are two interesting thresholds, r~0.01 and r~0.003. 
 - nt: slow-roll consistency condition.
 - running: The value predicted by slow-roll inflation is a well-defined target.
 - non-Gaussianity: There are various thresholds, local fNL=1, equilateral fNL=1, slow-roll fNL
 - curvature: \Omega_K~0.0001.
 - Is there a threshold for ns, contributions from isocurvature modes, features, other inflationary observables?

2. Can we reach these thresholds in an ideal experiment, and if so can we reach them with CMB S4?

 - Is there hope to measure the largest angular scales from the ground? 
 - How far can we go in multipole space in polarization, i.e. how well do we understand polarized foregrounds 
   from small scale experiments?

3. Given the focus on inflation, neutrinos and dark energy, are we missing interesting observables/opportunities?

  -e.g. constraints on primordial magnetic fields