The relation between velocity dispersion and temperature in clusters - Limiting the velocity bias

Details The relation between velocity dispersion and temperature in clusters - Limiting the velocity bias The relation between velocity dispersion and temperature in clusters - Limiting the velocity bias

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...415l..17l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 415, no. 1, p. L17-L20.

Astronomy and Astrophysics

Astronomy

112

Dark Matter, Galactic Clusters, Radial Velocity, X Ray Astronomy, Gas Temperature, Particle Mass, Velocity Distribution

Scientific paper

The observed galaxy velocity dispersion in clusters of galaxies is compared with the X-ray temperature of the intracluster gas for a large sample of clusters. A strong correlation is found between the observables which is best fitted by the relation sigma = 332 +/- 52(kT) exp 0.6 +/- 0.1 km/s; here sigma is the rms radial velocity dispersion in the cluster, and kT is the gas temperature in keV. The relation is consistent with that expected from an isothermal model where both the gas and the galaxies are in hydrostatic equilibrium with the binding cluster potential, i.e., sigma varies as T exp 0.5. The observed relation is used to determine the best-fit average beta parameter for clusters, beta = sigma-squared/(kT/mu-m(p)), which describes the ratio of energy per unit mass in the galaxies to that in the gas (where mu-m(p) is the mean particle mass); we find beta = 0.94 +/- 0.08 (and beta(median) = 0.98). This implies that the galaxies and the gas trace the same cluster potential with approximately equal energy per unit mass (i.e., beta = 1).

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