Cluster Masses from CMB and Galaxy Weak Lensing

Details Cluster Masses from CMB and Galaxy Weak Lensing Cluster Masses from CMB and Galaxy Weak Lensing

2005-12-05

arxiv.org/abs/astro-ph/0512104v2

Phys.Rev.D73:063006,2006

Astronomy and Astrophysics

Astrophysics

PRD accepted; 18 pages, 7 figures

Scientific paper

10.1103/PhysRevD.73.063006

Gravitational lensing can be used to directly constrain the projected density profile of galaxy clusters. We discuss possible future constraints from lensing of the CMB temperature and polarization, and compare to results from galaxy weak lensing. We model the moving lens and kinetic SZ signals that confuse the temperature CMB lensing when cluster velocities and angular momenta are unknown, and show how they degrade parameter constraints. The CMB polarization cluster lensing signal is ~1 micro-Kelvin for massive clusters and challenging to detect; however it should be significantly cleaner than the temperature signal and may provide the most robust constraints at low noise levels. Galaxy lensing is likely to be much better for constraining cluster masses at low redshift, but for clusters at redshift z >~ 1 future CMB lensing observations may be able to do better.

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