Intracluster Comptonization of the CMB: Mean Spectral Distrortion and Cluster Number Counts

Details Intracluster Comptonization of the CMB: Mean Spectral Distrortion and Cluster Number Counts Intracluster Comptonization of the CMB: Mean Spectral Distrortion and Cluster Number Counts

1997-03-19

arxiv.org/abs/astro-ph/9703121v1

Astronomy and Astrophysics

Astrophysics

23 pages, Latex, 11 PostScript figures, 5 PostScript tables, to appear in ApJ

Scientific paper

10.1086/303845

The mean sky-averaged Comptonization parameter, y, describing the scattering of the CMB by hot gas in clusters of galaxies is calculated in an array of flat and open cosmological and dark matter models. The models are globally normalized to fit cluster X-ray data, and intracluster gas is assumed to have evolved in a manner consistent with current observations. We predict values of y lower than the COBE/FIRAS upper limit. The corresponding values of the overall optical thickness to Compton scattering are < 10^{-4} for relevant parameter values. Of more practical importance are number counts of clusters across which a net flux (with respect to the CMB) higher than some limiting value can be detected. Such number counts are specifically predicted for the COBRAS/SAMBA and BOOMERANG missions.

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