UMICH-2015: CMB-Lensing break-out session 1

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Lensing autospectrum

Alex V. leading discussion, ~15 min

Alex's preliminary slides for discussion

  1. CMB lensing intro
  2. Sensitivity to neutrino mass and other parameters (w, $\Omega_k$)
  3. Foreground challenges
    • Extragalactic polarized sources
      • How big of an issue can they be? The CMBPol study 0811.3916 shows they give small biases under conservative assumptions, particularly if the resolution is high enough to find sources
      • They can also be projected out of the estimator (bias-hardening)
    • Galactic dust
      • Biases from nonzero connected four-point function at high-ell? e.g. 1207.0508
    • Instrumental systematics
      • gain variations, monopole leakagge, quadrupole leakage, pointing/beam offsets
  4. Impact of nonlinear growth of structure?
  5. How important are better optical depth measurements for m_\nu constraints from CMB lensing?
  6. Can we reconstruct large-scale lensing modes from a patchwork of small-area observations? Related issue: requirements on relative calibration across patches?

The following figures are to explain:

  • The sensitivity of the lensing potential to varying neutrino mass
  • The complementary orientation of degeneracy structure in the omegam-Mnu plane from DESI BAO

PanKnoxFig1.png The primary impact of neutrino mass on low-redshift probes of cosmology (including lensing) is the increase in expansion rate at z > 1 and its decrease at z < 1 (due to need to decrease the cosmological constant value to keep distance to last scattering unchanged. PanKnoxFig4.png Rl is the fractional change in the lensing power spectrum per meV change in neutrino mass PanKnoxFig5.png

  • omegam increases lensing power while Mnu decreases it hence they are positively correlated for CMB-S4.

Lensing by individual DM halos

Neelima leading discussion - ~10 min

  1. mass estimate forecasts
  2. instrument requirements
  3. systematic/foreground challenges

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