scholarly journals Radio Sources Observed with the Culgoora Circular Array

1995 ◽  
Vol 48 (1) ◽  
pp. 143 ◽  
Author(s):  
OB Slee
Keyword(s):  
Electronic Version ◽  
Radio Sources ◽  
Clusters Of Galaxies ◽  
Circular Array ◽  
Abell Clusters ◽  
On Line

I present a final updated and recalibrated list of sources that were observed with the Culgoora circular array in the interval 1970~1984. The present list contains all the sources that were contained in the Culgoora-1, 2, 3 Lists plus additional sources resulting from a survey of 353 Abell clusters of galaxies. The electronic version of the Culgoora List, with appropriate documentation, is available from the Einstein On-Line Service.

Radio Data on Clusters of Galaxies from the Culgoora Circular Array

1983 ◽  
Vol 5 (1) ◽  
pp. 114-129 ◽  
Author(s):  
O. B. Slee ◽  
Betty C. Siegman
Keyword(s):  
Low Frequency ◽  
Radio Sources ◽  
Clusters Of Galaxies ◽  
Circular Array ◽  
Radio Data ◽  
Contour Maps ◽  
Flux Data ◽  
Intensity Measurements ◽  
Half Power ◽  
Selection Of

The Culgoora circular array (CCA) is a 3-km-diameter ring of 96 reflectors operating at 80, 160 and 327 MHz. It has an effective collecting area of ~ 6000 m2 and achieves angular resolutions (full half-power beamwidths) of 3’.70, 1 ‘.85 and 0’.92 at the three operating frequencies. During the interval 1978-1981 we have used the CCA to make 80 and 160 MHz measurements of a comprehensive selection of radio sources which were detected during various complete surveys of clusters of galaxies (see Table 1). We have combined our low-frequency intensity measurements with other available higher-frequency flux data to compute accurate radio spectra. The 160 MHz contour maps for many of the cluster fields were used to find positions and angular sizes for the associated radio sources.

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.

Radio Sources with Wide-Angle Tails in Abell Clusters of Galaxies

1976 ◽  
Vol 205 ◽  
pp. L1 ◽  
Author(s):  
Frazer N. Owen ◽  
Lawrence Rudnick
Keyword(s):  
Radio Sources ◽  
Wide Angle ◽  
Clusters Of Galaxies ◽  
Abell Clusters

scholarly journals Radio Properties of Abell Clusters

1978 ◽  
Vol 79 ◽  
pp. 137-147 ◽  
Author(s):  
C. Lari ◽  
G.C. Perola
Keyword(s):  
Radio Sources ◽  
Clusters Of Galaxies ◽  
Abell Clusters ◽  
Radio Power

Since the early 60's the association of some radio sources with rich clusters of galaxies was noted (Mills, 1960; van den Bergh, 1961) and subsequent investigations concentrated mostly on the radio properties of clusters in the Abell catalogue. This paper is confined to this subject, although one should bear in mind the importance of associations with other scales of clustering which do not appear as entries of that catalogue. in this paper we shall use HO = 100 km sec−1 and the radio power P in WHz−1 at 408 MHz.

ROSATX‐Ray Observations of Abell Clusters with Wide‐Angle Tailed Radio Sources

1997 ◽  
Vol 474 (2) ◽  
pp. 580-597 ◽  
Author(s):  
P. L. Gomez ◽  
J. Pinkney ◽  
J. O. Burns ◽  
Q. Wang ◽  
F. N. Owen ◽  
...  
Keyword(s):  
Radio Sources ◽  
Wide Angle ◽  
Abell Clusters

scholarly journals Synthesis Observations of Southern Radio Sources at 1410 MHz with the Parkes Interferometer. I. Instrument, Reduction, and Preliminary Results

1973 ◽  
Vol 26 (5) ◽  
pp. 661 ◽  
Author(s):  
UJ Schwarz ◽  
DJ Cole ◽  
D Morris
Keyword(s):  
Data Processing ◽  
Computer Control ◽  
Radio Sources ◽  
Preliminary Results ◽  
On Line ◽  
Optical Identifications

Modifications to the Parkes interferometer are described which allow synthesis observations to be made while still retaining the flexibility of frequent baseline changes. Details are given of the receiver with a phase stabilizing device and its performance, on-line computer control, and data processing. Preliminary observations with a resolution of l' of the two sources PKS 2152-69 and 2356-61 and possible optical identifications are discussed briefly.

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.

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