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For refcode 1999ApJ...520...78H:
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1999ApJ...520...78H Observational Tests of the Mass-Temperature Relation for Galaxy Clusters DONALD J. HORNER AND RICHARD F. MUSHOTZKY Laboratory for High Energy Astrophysics, NASA/GSFC, Code 662, Greenbelt, MD 20771 AND CALEB A. SCHARF Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 Received 1998 September 23; accepted 1999 March 1 ABSTRACT We examine the relationship between the mass and X-ray gas temperature of galaxy clusters using data drawn from the literature. Simple theoretical arguments suggest that the mass of a cluster is related to the X-ray temperature as M is proportional to T_X_^3/2^. Virial theorem mass estimates based on cluster galaxy velocity dispersions seem to be accurately described by this scaling with a normalization consistent with that predicted by the simulations of Evrard, Metzler, and Navarro. X-ray mass estimates that employ spatially resolved temperature profiles also follow a T_X_^3/2^ scaling although with a normalization about 40% lower than that of the fit to the virial masses. However, the isothermal {beta}- model and X-ray surface brightness deprojection masses follow a steeper is proportional to T_X_^1.8-2.0^ scaling. The steepness of the isothermal estimates is due to their implicitly assumed dark matter density profile of {rho}(r)is proportional to r^-2^ at large radii, whereas observations and simulations suggest that clusters follow steeper profiles [e.g., {rho}(r)is proportional to r^-2.4^]. Subject headings: galaxies: clusters: general-X-rays: galaxies
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