The 1400-MHz luminosity function for Abell clusters of galaxies

1975 ◽  
Vol 195 ◽  
pp. 593 ◽  
Author(s):  
F. N. Owen
Keyword(s):  
Luminosity Function ◽  
Clusters Of Galaxies ◽  
Abell Clusters

scholarly journals Evolution of the Cluster X-Ray Luminosity Function

1980 ◽  
Vol 92 ◽  
pp. 231-231
Author(s):  
Stephen C. Perrenod
Keyword(s):  
Power Law ◽  
Luminosity Function ◽  
Mass Function ◽  
Mass Relation ◽  
Clusters Of Galaxies ◽  
Supply Rate ◽  
X Ray ◽  
Abell Clusters ◽  
Number Counts ◽  
Gas Supply

I predict the evolution of the X-ray luminosity function of clusters of galaxies. Predominantly, I treat the assumption that galaxies form first, then cluster purely due to gravitation. I show that the richness distribution of Abell clusters favors this scenario, rather than the protocluster hypothesis. The luminosity function is produced by combining a generalized (for all Ω) Press-Schechter evolutionary mass function for clusters (derived herein) with a power law X-ray luminosity-mass relation; a power law relation is supported by observations of low-redshift clusters.I find very steep evolution in the luminosity function, and thus in the source counts, for large Ω, and moderate evolution for small Ω. For a variety of models for the gas supply rate to the intracluster medium, the evolution of the luminosity function does not vary greatly. Thus it appears that the Ω, dependence will dominate and that number counts of X-ray clusters will yield cosmological information. The power of a test of Ω with an evolving luminosity function is considerably enhanced relative to a test which involves solely global cosmological effects on a non-evolving population. This occurs because of the well-known result that, at late times, clustering tends to proceed slowly for universes of small Ω and rapidly for large Ω.

scholarly journals A Radio Study of Abell Clusters

1977 ◽  
Vol 30 (4) ◽  
pp. 509 ◽  
Author(s):  
BY Mills ◽  
DG Hoskins
Keyword(s):  
Radio Source ◽  
Luminosity Function ◽  
Radio Sources ◽  
Clusters Of Galaxies ◽  
Multiple Sources ◽  
Radio Observatory ◽  
Cluster Membership ◽  
Abell Clusters

A search for radio sources close to 247 clusters of galaxies in the Abell catalogue has been carried out at the Molonglo Radio Observatory at a frequency of 408 MHz. A list of 116 sources near 89 clusters is given, identifications have been made and criteria for cluster membership have been established. A cluster luminosity function is derived in the range 1()23_1025 WHz-l SCi, and spectra have been obtained for sources in 25 clusters utilizing published surveys made at other frequencies. It is found that there is no correlation between the richness of a cluster and its inclusion of at least one radio source, but those clusters containing multiple sources are significantly richer than average.

scholarly journals Catalogue of Clusters that are Members of Superclusters

1983 ◽  
Vol 104 ◽  
pp. 185-186
Author(s):  
M. Kalinkov ◽  
K. Stavrev ◽  
I. Kuneva
Keyword(s):  
Standard Deviation ◽  
Correlation Coefficient ◽  
The Other ◽  
Clusters Of Galaxies ◽  
Number Of Clusters ◽  
Abell Clusters ◽  
The Mean ◽  
Abell Cluster ◽  
Image Position

An attempt is made to establish the membership of Abell clusters in superclusters of galaxies. The relation is used to calibrate the distances to the clusters of galaxies with two redshift estimates. One is m10, the magnitude of the ten-ranked galaxy, and the other is the “mean population,” P, defined by: where p = 40, 65, 105 … galaxies for richness groups 0, 1, 2 …, and r is the apparent radius in degrees given by: The first iteration for redshift, z1, is obtained from m10 alone: The standard deviation for Eq. (1) is 0.105, the number of clusters with known velocities is 342 and the correlation coefficient between observed and fitted values is 0.921. With zi from Eq. (1), we define Cartesian galactic coordinates Xi = Rih−1 cosBi cosLi, Yi = Rih−1 cosBi sinLi, Zi = Rih−1 sinBi for each Abell cluster, i = 1, …, 2712, where Ri is the distance to the cluster (Mpc), and Ho = 100 h km s−1 Mpc−1.

Redshifts of radio galaxies in Abell clusters of galaxies

1988 ◽  
Vol 95 ◽  
pp. 1 ◽  
Author(s):  
Frazer N. Owen ◽  
Richard A. White ◽  
Harley A., Jr. Thronson
Keyword(s):  
Radio Galaxies ◽  
Clusters Of Galaxies ◽  
Abell Clusters

Faraday rotation from Abell clusters of galaxies

1989 ◽  
Vol 347 ◽  
pp. 144 ◽  
Author(s):  
G. S. Hennessy ◽  
F. N. Owen ◽  
J. A. Eilek
Keyword(s):  
Faraday Rotation ◽  
Clusters Of Galaxies ◽  
Abell Clusters

scholarly journals Space Distribution of the Richest Abell Clusters of Galaxies

1988 ◽  
Vol 130 ◽  
pp. 533-533
Author(s):  
M Kalinkov ◽  
I Kuneva
Keyword(s):  
Space Distribution ◽  
List Type ◽  
Clusters Of Galaxies ◽  
Type Number ◽  
Abell Clusters

We discuss four samples from the Abell (1958) catalog of clusters of galaxies. Our samples are drawn out from the Abell sample and all clusters have richness 2 and 3. With Ho = 100 km/s/Mpc and qo = +1, we examine the following volumes, defined for both galactic hemispheres: (i)RG 3: b 40° for 0° < 1 360° and b 30° for 90° < 1 240°, distance 300 < R < 750 Mpc, N = 35 clusters, 30 of which with known redshift;(ii)RG 3: b −35° for 15° < 1 232°, 150 < R < 600 Mpc, N = 15 (13);(iii)RG 2: b and 1 as (i), 60 < R < 525 Mpc, N = 110 (55);(iv)RG 2: b and 1 as (ii), 120 < R < 600 Mpc, N = 102(14).

scholarly journals UHURU Results on Extragalactic X-Ray Sources

1973 ◽  
Vol 55 ◽  
pp. 171-183 ◽  
Author(s):  
Edwin M. Kellogg
Keyword(s):  
High Latitude ◽  
Luminosity Function ◽  
Optical Data ◽  
Clusters Of Galaxies ◽  
X Rays ◽  
Total Contribution ◽  
X Ray ◽  
Normal Galaxies ◽  
X Ray Background ◽  
Individual Galaxies

Data from the UHURU satellite have provided a list of more than forty high latitude sources (|b| > 20°). X-rays have been detected from among the nearest normal galaxies, giant radio galaxies, Seyferts, QSOs and clusters of galaxies. The cluster sources appear to be extended by several hundred kiloparsecs as well as being very luminous. These cluster sources have systematic differences in their X-ray spectra from individual galaxies.About twenty sources are not reliably identified so far. A few of these are located near undistinguished 3C or MSH radio sources. The rest are either located near distant clusters or undistinguished bright galaxies, or are too far south, so that we have not sufficient optical data to allow a thorough search for possible association with clusters or unusual individual galaxies.The luminosity function for weak, high latitude X-ray sources is determined, and the contribution of sources just below the UHURU threshold of detectability to observed fluctuations in the diffuse X-ray background is evaluated. The total contribution of all observed types of extragalactic sources to the X-ray background is estimated.

Sign in / Sign up

Export Citation Format

Share Document