UMICH-2015: Dark Energy / Gravity / Dark Matter break-out session 3
From CMB-S4 wikiJump to navigationJump to search
Diffuse SZ effects / Mapping momentum
- 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):
- How do forecasts on Dark Matter annihilation change when including foregrounds?
- How much can we tighten the constraints on <sigmav>/m by adding prior information on As from other observables?
- What other dark matter scenarios can we learn about from the CMB? (baryon/dark matter interactions, a complex dark sector, dark matter scattering with neutrinos, other models?)