3C 295

B1409+524

Basic Data
S178 Alpha FR Class ID Spectrum Best z mag. LAS lg P178 D
91.00.63IICD Gal0.4599R(c) = 18.92 5.8027.48 26.5

Image:


Size: 15.4 × 15.4 arcsec²
LUT: Logarithmic
Beam: 0.20 arcsec
Frequency: 8711 MHz
Method: CLEAN Ո>0.20
Telescope: VLA A
Credits: Perley & Taylor (1991)

3C 295 is the most powerful DRAGN in our sample, only slightly less luminous than Cygnus A. It is identified with the central cD galaxy in the rich cluster 1410+5226, usually known as the 3C 295 cluster. Henry & Henriksen (1986) show an X-ray image from the Einstein HRI, and argue that there is a cooling flow in the cluster.

The DRAGN is quite small, about the size of the optical image of the host galaxy. It is embedded in the X-ray core of the cluster. Perley & Taylor find that the cluster gas causes extreme Faraday Rotation.

The relatively "fat" SE lobe resembles that in Cyg A, in that it is marked by a bright ridge around the eastern boundary. The SE hotspot forms a resolved ridge parallel to the main axis, while the NW hotspot is very compact. There is a curious protrusion of intermediate brightness to the east of this hotspot, seen more clearly in the our supplementary high-resolution 15 GHz image on the Other Images page.


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Page created: 2009 Apr 8 00:59:19
J. P. Leahy
jpl@jb.man.ac.uk