Astronomy and Astrophysics – Astrophysics
Scientific paper
1998-07-11
Astrophys.J. 509 (1998) 544-550
Astronomy and Astrophysics
Astrophysics
19 pages, accepted for publication in ApJ, Part 1
Scientific paper
10.1086/306520
We describe a theoretical framework to compute the cluster gas distribution in hydrostatic equilibrium embedded in a class of spherical dark matter halo potentials. Unlike the conventional isothermal $\beta$-model, the present method provides a physical basis to directly probe the shape of dark matter halo from the observed X-ray surface brightness and temperature profiles of clusters of galaxies. Specifically, we examine the extent to which the resulting gas density and X-ray surface brightness profiles are sensitive to the inner slope of the dark matter halo density and other more realistic effects including the self-gravity of the gas and the polytropic equation of state. We also discuss a practical strategy to apply the present methodology to the actual cluster profiles from future X-ray observations.
Makino Nobuyoshi
Sasaki Shin
Suto Yasushi
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