Ravi Sheth  (Pittsburg Univ. /Univ. of Pennsylvania)

The Halo Model of Large Scale Structure

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  The halo model has become the standard framework within which to interpret measurements of clustering in the Universe. In addition to allowing one to model the distribution of the mass, velocity, momentum, temperature, and pressure fields on both linear and nonlinear scales, it provides a simple way to understand why the galaxy distribution is a biased tracer of dark matter, so it is vital for interpreting the distribution of galaxies observed in surveys such as the Sloan Digital Sky Survey. Therefore, it is the ideal framework within which to interpret measurements of weak lensing, the thermal and kinematic Sunyaev-Zeldovich effects, and how galaxy clustering depends on galaxy type, both in real and in redshift space. I will discuss the background of the model, and review some of its applications.