UMICH-2015: Neutrino and Light Relativisic Species break-out session 1

From CMB-S4 wiki
Revision as of 14:21, 17 September 2015 by Drgreen (talk | contribs)
Jump to navigationJump to search

Wiki navigation

Return to main workshop page

Return to Neutrino and Light Relativisic Species sessions page

Clear science target - A massless field in thermal equilibrium with the Standard model leads to ΔNeff > 0.027
For thermal decoupling above 100 GeV 
a real scalar produces ΔNeff = 0.027
a Weyl fermion produces ΔNeff = 0.047 (Dirac : 0.094)
a vector field produces ΔNeff = 0.054
With 106 detectors and fsky = 0.75, forecasts of σNeff =0.013 (see e.g. arXiv
1402.4108).
Model independent theory motivation - Is this realistic experimentally?
What are the trade-offs for other science goals to achieve this sensitivity
What is missing from the forecast that could significantly reduce the sensitivity?
More general science targets -- axion-like particles, late decays of massive fields (before or after BBN), decaying Dark matter
How well can be break degeneracies?
E.g. Want to separate NeffCMB from Yp
Forecasts with both varying give σNeff = 0.048 and σYp = 0.0027 (see arXiv:1508.06342)
In principle allows us to distinguish effects at recombination from changes to BBN
What role does CMB lensing play?
For Neff, delensing E-modes improves constraints significantly (sharpens peaks - improves phase shift measurement)
Can it help break degeneracies in other models (e.g. decaying dark matter) ?
Planck 2015 versus CMB Stage IV (2 different marginalizations - see arXiv
1508.06342)

Neff.png