Computer Science – Numerical Analysis
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...429..545f&link_type=abstract
The Astrophysical Journal, vol. 429, no. 2, pt. 1, p. 545-553
Computer Science
Numerical Analysis
15
Comets, Cosmology, Density Distribution, Galactic Clusters, Intergalactic Media, Isothermal Processes, Light (Visible Radiation), Static Models, Temperature Distribution, Ginga Satellite, Numerical Analysis, Rosat Mission, Tenma Satellite, X Ray Imagery, X Ray Spectra
Scientific paper
In this article we demonstrate, for the first time, how a physically motivated static model for both the gas and galaxies in the Coma Cluster of galaxies can jointly fit all available X-ray and optical imaging and spectroscopic data. The principal assumption of this nonpolytropic model (Cavaliere & Fusco-Femiano 1981, hereafter CFF), is that the intracluster gas temperature is proportional to the square of the galaxy velocity dispersion everywhere throughout the cluster; no other assumption about the gas temperature distribution is required. After demonstrating that the CFF nonpolytropic model is an adequate representation of the gas and galaxy distributions, the radial velocity dispersion profile, and the gas temperature distribution, we derive the following information about the Coma Cluster: 1. The central temperature is about 9 keV and the central density is 2.8 x 10-3/cm3 for the X-ray emitting plasma; 2. The binding mass of the cluster is approximately 2 x 1015 solar mass within 5 Mpc for (H0 = 50 km/sec/Mpc), with a mass-to-light ratio of approximately 160 solar mass/solar luminosity; 3. The contribution of the gas to the total virial mass increases with distance from the cluster center, and we estimate that this ratio is no greater than approximately 50% within 5 Mpc. The ability of the CFF nonpolytropic model to describe the current X-ray and optical data for the Coma Cluster suggests that a significant fraction of the thermal energy contained in the hot gas in this as well as other rich galaxy clusters may have come from the interaction between the galaxies and the ambient cluster medium. interaction between the galaxies and the ambient cluster medium.
Fusco-Femiano Roberto
Hughes John Patrick
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