========================================================================== J/AJ/104/2078 cD Galaxy in Abell 2107 (Oegerle+ 1992) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1 ========================================================================== Query from: http://vizier.u-strasbg.fr/cgi-bin/VizieR?-source=J/AJ/104/2078 ==========================================================================
drwxr-xr-x 11 cats archive 4096 Dec 1 11:14 [Up] drwxr-xr-x 2 cats archive 4096 May 12 09:54 [TAR file] -rw-r--r-- 1 cats archive 465 Jan 6 1999 .message -r--r--r-- 1 cats archive 3057 Jan 6 1999 ReadMe -rw-r--r-- 1 cats archive 613 Sep 19 2007 +footg5.gif -rw-r--r-- 1 cats archive 2299 Mar 5 2008 +footg8.gif -r--r--r-- 1 cats archive 2748 Dec 2 1993 table1
Beginning of ReadMe : J/AJ/104/2078 cD Galaxy in Abell 2107 (Oegerle+ 1992) ================================================================================ Structure, rotation, and the peculiar velocity cD galaxy in Abell 2107 OEGERLE W.R., HILL J.M. <Astron. J. 104, 2078 (1992)> =1992AJ....104.2078O ================================================================================ ADC_Keywords: Clusters, galaxy; Radial velocities Abstract: As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.
© UDS/CNRS