Determining the Gas Mass ffraction as a Function of Redshift in Galaxy Clusters Using X-ray and Sunyaev Zel'dovich Effect Observations

Details Determining the Gas Mass ffraction as a Function of Redshift in Galaxy Clusters Using X-ray and Sunyaev Zel'dovich Effect Observations Determining the Gas Mass ffraction as a Function of Redshift in Galaxy Clusters Using X-ray and Sunyaev Zel'dovich Effect Observations

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.3408h&link_type=abstract

American Astronomical Society, HEAD meeting #11, #34.08; Bulletin of the American Astronomical Society, Vol. 41, p.711

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Using Chandra X-ray data and Suyaev Zel'dovich Effect (SZE) observations taken with the Sunyaev Zel'dovich Array, we make direct measurements of the gas mass fraction in galaxy clusters as a function of redshift for a sample of clusters spanning (z=0.09-1.06). The advantage of using a joint X-ray/SZE analysis approach is that we are able to directly determine the angular diameter distance of the cluster, and therefore determine cluster masses without assuming a cosmology. Under the assumption of non-evolving gas mass fractions, X-ray measurements have been used to place tight constraints on cosmological parameters. Through this joint SZE and X-ray analysis we can test this assumption directly. We apply here physically motivated models we developed to describe the density, temperature, and pressure of the intra-cluster medium, using a polytropic equation of state to describe the cluster properties at large radii. These models also incorporate a taper function to fit the inner regions in cool core clusters. We present here the results of our analysis, where we have measured the cluster gas and total mass -- and hence gas mass fraction -- for this moderately large sample.

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