UMICH-2015: Response to Inflation Action Items

From CMB-S4 wiki
Revision as of 12:20, 2 November 2015 by Flauger (talk | contribs)
Jump to navigationJump to search

Action Items: updated list, with names (November 2, 2015)

  • Start writing (making a strong case for r): RF and SS will get started right away.
  • Study prospects for r and nt for various configurations and values of r (Fisher matrix forecasts including foregrounds that will feed into more detailed simulations) -- RF
  • Study possibility to establish departure from scale invariance even for extended parameters space for both S3 and S4 -- RF
  • Quantify improvements on other inflationary observables (running, non-Gaussianity, etc. while varying neutrino mass/Neff) -- RF
  • Given the improvements on fNL, are there interesting models that CMB S4 could see hints for (e.g. modulated reheating): Joel Meyers
  • Quantify dependence of error bars on lmin

Several observables display a dependence on lmin that motivates lmin=14. One example is the optical depth.

Tauvslmin.png

It is shown as a function of lmin for two values of the optical depth and two reionization histories. Parameters degenerate with it inherit the strong dependence. The reionization histories corresponding to the various curves are shown in the next plot. This is largely independent of the reionization history.

Xe.png

The multipole range that contains most of the information does not significantly depend on the reionization history but does depend on the optical depth. The effect of the different reionization histories on the angular power spectra is shown in the next plot.

Clee dzr.png

  • Think about science drivers that would affect design of experiment (e.g. absolute calibration of polarization angles) -- ?

Light axions with masses between 10^-33 eV and 4x10^-28 eV (not the QCD axion) would lead to an isotropic rotation by ~9 arcmin (independent of the axion decay constant). This would be rotated away by EB nulling. (The mass range is such that they oscillate between recombination and today, but not long before recombination).

The absolute polarization angles are currently typically calibrated to around 1 degree, and it is difficult to do much better. To detect such axions or rule them out, one would have to calibrate the polarization angles at ~3 arcmin.

A very neat idea to achieve this goal was recently proposed in http://arxiv.org/abs/1505.07033

  • Isocurvature forecasts -- no obvious targets, but there should be some quantification. How to parameterize? -- Julien Lesgourgues