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Journal ArticleDOI

The dynamics and structure of rich clusters of galaxies. I : Velocity data

Peter F. Teague, +2 more
- 01 Apr 1990 - 
- Vol. 72, Iss: 4, pp 715-753
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TLDR
In this paper, an extensive spectroscopic study of 10 rich southern X-ray clusters of galaxies is presented, where between 40 and 200 redshifts have been obtained in the field of each of the clusters, which cover a wide range of morphological types and richnesses.
Abstract
An extensive spectroscopic study of 10 rich southern X-ray clusters of galaxies is presented. Between 40 and 200 redshifts have been obtained in the field of each of the clusters, which cover a wide range of morphological types and richnesses. Applying rigorous statistical analyses to the total data base of 1000 precise radial velocities provides the necessary information to undertake a thorough dynamical investigation of these individual clusters and of cluster systems in general. 92 refs.

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Journal ArticleDOI

The Mass Function of an X-Ray Flux-Limited Sample of Galaxy Clusters

TL;DR: In this article, a new X-ray-selected and Xray flux-limited galaxy cluster sample is presented, based on the ROSAT All-Sky Survey, the 63 brightest clusters with galactic latitude |bII|? 20? and flux fX(0.1-2.4keV)? 2? 10-11ergss-1cm-2 have been determined utilizing intracluster gas density profiles, derived mainly from ROSAT PSPC pointed observations, and gas temperatures, as published mainly from ASCA observations.

The mass function of an X-ray flux-limited sample of galaxy clusters

TL;DR: In this article, a new X-ray-selected and Xray flux-limited galaxy cluster sample is presented, based on the ROSAT All-Sky Survey, the 63 brightest clusters with galactic latitude |bII|? 20? and flux fX(0.1-2.4keV)? 2? 10-11ergss-1cm-2 have been determined utilizing intracluster gas density profiles, derived mainly from ROSAT PSPC pointed observations, and gas temperatures, as published mainly from ASCA observations.
Journal ArticleDOI

Optical mass estimates of galaxy clusters

TL;DR: In this paper, the mass of 170 nearby clusters (z ≤ 0.15) is computed by applying the virial theorem to the member galaxies, assuming that mass follows the galaxy distribution and that clusters are not far from a situation of dynamical equilibrium.
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