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

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==Spectral Index, Running, Non-Gaussianity, ...==
 
==Spectral Index, Running, Non-Gaussianity, ...==
  
1. For which observables do we have well-motivated theory thresholds?
+
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.  
+
* r: One may argue there are two interesting thresholds, r~0.01 and r~0.003.  
  - nt: slow-roll consistency condition.
+
* nt: slow-roll consistency condition.
  - running: The value predicted by slow-roll inflation is a well-defined target.
+
* 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
+
* non-Gaussianity: There are various thresholds, local fNL=1, equilateral fNL=1, slow-roll fNL
  - curvature: \Omega_K~0.0001.
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* curvature: \Omega_K~0.0001.
  - Is there a threshold for ns, contributions from isocurvature modes, features, other inflationary observables?
+
* 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?
+
2. ''Can we reach these thresholds in an ideal experiment, and if so can we reach them with CMB S4?''
  
  -e.g. constraints on primordial magnetic fields
+
* 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?
 +
* How much of the sky and what beam size should one ideally use for the different observables?
 +
* How well do foregrounds have to be controlled?
 +
 
 +
 
 +
 
 +
3. ''Given the focus on inflation, neutrinos and dark energy, are we missing interesting observables/opportunities?''
 +
 
 +
* e.g. constraints on primordial magnetic fields

Revision as of 16:33, 16 September 2015

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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?
  • How much of the sky and what beam size should one ideally use for the different observables?
  • How well do foregrounds have to be controlled?


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

  • e.g. constraints on primordial magnetic fields