paper

ABELL 2163: Temperature, Mass, and Hydrostatic Equilibrium

arXiv:astro-ph/9506090 · doi:10.1086/176668

Abstract

Using ASCA data, we have measured the electron temperature in A2163 out to 1.5h^{-1} Mpc (10a_x) from the center, in three radial bins. The temperatures are 12.2+1.9-1.2 keV, 11.5+2.7-2.9 keV and 3.8+1.1-0.9 keV (90%) in the 0-3 a_x (0-3.5'), 3-6 a_x and 6-13 a_x spherical shells, respectively. Applying the hydrostatic equilibrium and spherical symmetry assumptions and using these data together with the Ginga spectral and the Rosat imaging data, we were able to severely limit the possible binding mass distribution of the generic form rho=rho_0 (1+r^2/a_b^2)^{-n/2}. All the allowed binding mass profiles are steeper than the gas density profiles and mass profiles with the same slope as gas are excluded at a greater than 99% confidence. The total mass inside 0.5h^{-1} Mpc is 4.3+-0.5 10^14 h^{-1} Msun, of which 0.074 h^{-3/2} is gas while inside 1.5h^{-1} Mpc the mass is 1.07+-0.13 10^15 h^{-1} Msun. We note that in the cluster outer part, the timescale for electron-ion temperature equlibration is comparable to the merger timescale, so the measured electron temperature may give an underestimate of the gas pressure there. Otherwise, if our low temperature is indeed representative of the gas temperature in the outer shell, the cluster atmosphere should be convectionally unstable and gas turbulence should exist. Bulk motions of the gas are also expected during the merger. Their existense would increase the total gas pressure above that indicated by the observed temperature. Thus, failure of the "gas follows dark matter" model, favored by hydrodynamic simulations, may be due to the neglect of these phenomena, leading to an underestimate of the total density at large radii.

19 pages, 5 postscript figures, uses aaspp.sty. Accepted for ApJ

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