Determination of the mass distribution in rich clusters from imaging x-ray spectroscopy

Details Determination of the mass distribution in rich clusters from imaging x-ray spectroscopy Determination of the mass distribution in rich clusters from imaging x-ray spectroscopy

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aipc..336..231m&link_type=abstract

Dark matter. AIP Conference Proceedings, Volume 336, pp. 231-242 (1995).

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13

Dark Matter, X-Ray, Galaxy Clusters

Scientific paper

We discuss the use of x-ray imaging spectroscopy to derive the mass profiles of rich clusters of galaxies. Using the recent ASCA spectra of A496, A1795, and A2199 we find that the masses are formally constrained at R~1 Mpc to a statistical precision of a few percent and that all 3 of these systems have very similar gas to total mass ratios of ~20%. These results are in good agreement with the available Rosat results but of considerably higher precision. The derived optical velocity dispersions from our model potentials are in good agreement with the published optical data. We conclude, based on the available numerical simulations and consideration of other likely sources of pressure (magnetic fields, turbulence and cosmic rays) that the mass derived from this technique is not subject to large error.

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