Difference between revisions of "UMICH-2015: Dark Energy / Gravity / Dark Matter break-out session 3"

From CMB-S4 wiki
Jump to: navigation, search
Line 4: Line 4:
 
[[UMICH-2015: Dark Energy / Gravity / Dark Matter|Return to  Dark Energy / Gravity / Dark Matter sessions page]]
 
[[UMICH-2015: Dark Energy / Gravity / Dark Matter|Return to  Dark Energy / Gravity / Dark Matter sessions page]]
  
'''Diffuse SZ effects / Mapping momentum/ Dark Matter'''
+
'''Diffuse SZ effects / Mapping momentum'''
  
 
Key questions:
 
Key questions:
Line 18: Line 18:
 
* SZ polarization: offers another way to constrain clusters optical depths. Plus several other nice things: CMB quadrupole vs redshift for example. The signal is small (~0.1 uK at the center of very massive clusters) but stacking approaches might work.
 
* SZ polarization: offers another way to constrain clusters optical depths. Plus several other nice things: CMB quadrupole vs redshift for example. The signal is small (~0.1 uK at the center of very massive clusters) but stacking approaches might work.
 
* SZ polarization from transverse motion of clusters: sensitive to the transverse component of the velocity field (hence, complementary to kSZ). Potentially very interesting but even smaller than the previous effect: suppressed by (v_t/c)^2. It should have a different frequency dependence though.
 
* SZ polarization from transverse motion of clusters: sensitive to the transverse component of the velocity field (hence, complementary to kSZ). Potentially very interesting but even smaller than the previous effect: suppressed by (v_t/c)^2. It should have a different frequency dependence though.
 +
 +
 +
'''Dark Matter''' (lead by Cora Dvorkin):
 +
 +
Questions:

Revision as of 14:51, 17 September 2015

Wiki navigation

Return to main workshop page

Return to Dark Energy / Gravity / Dark Matter sessions page

Diffuse SZ effects / Mapping momentum

Key questions:

  • Which of those measurements is realistic? How to implement proper forecasts?
  • What parameters space should be explored?
  • How these probes compare to others (e.g. future galaxy surveys) in terms of constraints?

Some possible promising/interesting SZ topics:

  • kSZ pairwise statistics: promising with current data. It should be very powerful with CMB-S4.
  • kSZ via cross correlation with reconstructed velocity fields (see several papers from Shirley Ho, David Spergel and others). As above, it's already promising with current data, compelling in the future.
  • SZ polarization: offers another way to constrain clusters optical depths. Plus several other nice things: CMB quadrupole vs redshift for example. The signal is small (~0.1 uK at the center of very massive clusters) but stacking approaches might work.
  • SZ polarization from transverse motion of clusters: sensitive to the transverse component of the velocity field (hence, complementary to kSZ). Potentially very interesting but even smaller than the previous effect: suppressed by (v_t/c)^2. It should have a different frequency dependence though.


Dark Matter (lead by Cora Dvorkin):

Questions: