Difference between revisions of "LBNL-2016: Inflation Summary"

From CMB-S4 wiki
Jump to navigationJump to search
Line 24: Line 24:
 
==Currently needed==
 
==Currently needed==
  
* Section on isocurvature modes
+
 
 
* Realistic forecasts for:
 
* Realistic forecasts for:
 
** tensor-to-scalar ratio (first version from Victor Buza, Colin Bischoff, John Kovac in the draft)
 
** tensor-to-scalar ratio (first version from Victor Buza, Colin Bischoff, John Kovac in the draft)
** tensor spectral index
+
** tensor spectral index, running
 
** scalar spectral index, running
 
** scalar spectral index, running
 
** non-Gaussianity, including BBB
 
** non-Gaussianity, including BBB
 +
* Section on isocurvature modes
 +
* Additional discussion on bispectrum
 +
* Discussion of trispectrum
 +
* Streamline various sections
  
 
==Open questions==
 
==Open questions==
  
* Should the inflation chapter  
+
Bigger picture questions
 +
* Should the inflation chapter be thought of as independent at some level? If so, it should likely include higher level discussion
 +
* CMB-S4 can only reach theoretically well motivated thresholds for r. As a consequence r is the main inflationary driver of the design, and the chapter is focused on primordial gravitational waves. Other aspects imply CMB-S4 will have high angular resolution. Should the discussion of constraints on the power spectrum, bispectrum,... be expanded?
 +
* Should the inflation chapter be focused on inflation or include implications of high-scale inflation for other areas of fundamental physics?
 +
 
 +
More detailed questions
 +
* How much time and effort should be spent on strawman models that produce B-mode power in excess of the inflationary signal?
 +
* Should various sections be moved or remain in the inflation chapter?
 +
** Constraints on the graviton
 +
** Birefringence
  
  

Revision as of 14:14, 7 March 2016

File:CMBS4inflation.pdf

Status of Inflation Chapter

  1. Introduction
  2. Implications of a detection of primordial gravitational waves with CMB-S4
    • The energy scale of inflation
    • Planckian field ranges and symmetries
    • Constraints on the graviton mass
    • Following up on a detection
  3. Lessons from upper limits
  4. CMB data products and simulations to achieve goals for PGW
  5. Improved constraints on primordial density perturbations
    • The power spectrum of primordial density perturbations
    • Higher order correlations
    • Isocurvature
  6. Constraints on curvature, cosmic birefringence, cosmic strings, axions,...
    • Spatial curvature
    • Cosmic Birefringence
    • Cosmic Strings
    • Anomalies
  7. Summary

Currently needed

  • Realistic forecasts for:
    • tensor-to-scalar ratio (first version from Victor Buza, Colin Bischoff, John Kovac in the draft)
    • tensor spectral index, running
    • scalar spectral index, running
    • non-Gaussianity, including BBB
  • Section on isocurvature modes
  • Additional discussion on bispectrum
  • Discussion of trispectrum
  • Streamline various sections

Open questions

Bigger picture questions

  • Should the inflation chapter be thought of as independent at some level? If so, it should likely include higher level discussion
  • CMB-S4 can only reach theoretically well motivated thresholds for r. As a consequence r is the main inflationary driver of the design, and the chapter is focused on primordial gravitational waves. Other aspects imply CMB-S4 will have high angular resolution. Should the discussion of constraints on the power spectrum, bispectrum,... be expanded?
  • Should the inflation chapter be focused on inflation or include implications of high-scale inflation for other areas of fundamental physics?

More detailed questions

  • How much time and effort should be spent on strawman models that produce B-mode power in excess of the inflationary signal?
  • Should various sections be moved or remain in the inflation chapter?
    • Constraints on the graviton
    • Birefringence


Wiki navigation

Return to main workshop page

Return to Inflation sessions page