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

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.

scholarly journals Extragalactic jets as probes of distant clusters of galaxies and the clusters occupied by bent radio AGN (COBRA) survey

2014 ◽  
Vol 10 (S313) ◽  
pp. 315-320
Author(s):  
Elizabeth L. Blanton ◽  
Rachel Paterno-Mahler ◽  
Joshua D. Wing ◽  
M. L. N. Ashby ◽  
Emmet Golden-Marx ◽  
...  
Keyword(s):  
Radio Galaxies ◽  
Radio Sources ◽  
Clusters Of Galaxies ◽  
Wide Range ◽  
Extragalactic Jets ◽  
Large Survey ◽  
Kinetic Mode ◽  
Group Environments ◽  
Initial Results ◽  
Quasars And Radio Galaxies

AbstractWe are conducting a large survey of distant clusters of galaxies using radio sources with bent jets and lobes as tracers. These radio sources are driven by AGN and achieve their bent morphologies through interaction with the surrounding gas found in clusters of galaxies. Based on low-redshift studies, these types of sources can be used to identify clusters very efficiently. We present initial results from our survey of 653 bent-double radio sources with optical hosts too faint to appear in the SDSS. The sample was observed in the infrared with Spitzer, and it has revealed ~200 distant clusters or proto-clusters in the redshift range z ~ 0.7 - 3.0. The sample of bent-doubles contains both quasars and radio galaxies enabling us to study both radiative and kinetic mode feedback in cluster and group environments at a wide range of redshifts.

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 Observations of Straight-angle Tailed Radio Galaxies in Rich Clusters of Galaxies

1996 ◽  
Vol 175 ◽  
pp. 349-350
Author(s):  
Aileen A. O'Donoghue ◽  
Jean A. Eilek ◽  
Frazer N. Owen
Keyword(s):  
Spectral Index ◽  
Radio Galaxies ◽  
Radio Sources ◽  
Clusters Of Galaxies ◽  
Data Set ◽  
Dynamical Properties

We have begun VLA observations of straight-angle tailed radio sources (SATs) at 1.5 and 4.8 GHz (L and C band) to achieve one arcsecond resolution at each frequency. This will provide a SAT data set similar to the O'Donoghue, Owen, and Eilek (1990) WAT data set with both total intensity and spectral index information. We will use these data to examine morphological and dynamical properties of straight-tailed radio sources in clusters of galaxies.

scholarly journals Theoretical Implications of Diffuse Non-Thermal Emission from Clusters of Galaxies

2002 ◽  
Vol 199 ◽  
pp. 141-148
Author(s):  
T.A. Enßlin
Keyword(s):  
Thermal Emission ◽  
Extreme Ultraviolet ◽  
Short Review ◽  
Radio Galaxies ◽  
High Energy ◽  
Clusters Of Galaxies ◽  
Thermal Electron ◽  
Electron Population ◽  
X Ray

A short review on theoretical implications of non-thermal emission (radio, extreme ultraviolet, high energy X-ray) from the intra-cluster medium is given. The origin of cluster radio halos and cluster radio relics is discussed within the framework of a network of processes producing a non-thermal electron population. Emphasis is given to the role of old, remnant, presently invisible relativistic plasma released by former radio galaxies.

scholarly journals THE ENVIRONMENT OFz> 1 3CR RADIO GALAXIES AND QSOS: FROM PROTO-CLUSTERS TO CLUSTERS OF GALAXIES?

2016 ◽  
Vol 826 (1) ◽  
pp. 46 ◽  
Author(s):  
J. P. Kotyla ◽  
M. Chiaberge ◽  
S. Baum ◽  
A. Capetti ◽  
B. Hilbert ◽  
...  
Keyword(s):  
Radio Galaxies ◽  
Clusters Of Galaxies

scholarly journals The correlation function of rich clusters of galaxies: a comparison of APM and Abell clusters

1992 ◽  
Vol 257 (1) ◽  
pp. 125-134 ◽  
Author(s):  
G. Efstathiou ◽  
G. B. Dalton ◽  
W. J. Sutherland ◽  
S. J. Maddox
Keyword(s):  
Correlation Function ◽  
Clusters Of Galaxies ◽  
Abell Clusters
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