Image:3C 295 | B1409+524 |
| S178 | Alpha | FR | Class | ID | Spectrum | Best z | mag. | LAS | lg P178 | D |
|---|---|---|---|---|---|---|---|---|---|---|
| 91.0 | 0.63 | II | CD | Gal | 0.4599 | R(c) = 18.92 | 5.80 | 27.48 | 26.5 |
Image:
| Size: | 15.4 × 15.4 arcsec² |
|---|---|
| LUT: | Logarithmic |
| Beam: | 0.20 arcsec |
| Frequency: | 8711 MHz |
| Method: | CLEAN Õˆÿ>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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