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waynehu

Professor, Department of Astronomy and Astrophysics
University of Chicago

Group Contact CV SnapShots
CMB Introduction '96   Intermediate '01   Polarization Intro '01   Cosmic Symphony '04   Polarization Primer '97   Review '02   Power Animations   Lensing   Power Prehistory   Legacy Material '96   PhD Thesis '95 Baryon Acoustic Oscillations Cosmic Shear Clusters
Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance
Cosmology I [legacy 321] Cosmology II [321] Current Topics [282] Galaxies and Universe [242] Radiative Processes [305] Research Preparation [307] GR Perturbation Theory [408] CMB [448] Cosmic Acceleration [449]


Rees-Sciama and Moving Halo Effects

The ISW effect is linear in the perturbations. Cancellation of the ISW effect on small scales leaves second order and non-linear analogues in its wake [Rees & Sciama, 1968]. From a single isolated structure, the potential along the line of sight can change not only from evolution in the density profile but more importantly from its bulk motion across the line of sight. In the context of clusters of galaxies, this is called the moving cluster effect [Birkinshaw & Gull, 1983]. More generally, the bulk motion of dark matter halos of all masses contribute to this effect [Tuluie & Laguna, 1995,Seljak, 1996b], and their clustering gives rise to a low level of anisotropies on a range of scales but is never the leading source of secondary anisotropies on any scale (see Plate 5a).

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