Flux data
Available Data Downloads
Images, Maps, Spectra and SEDs
Infrared data
Radio data
Optical data
X-Ray data
Chandra
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.153
22 14 25.78
-17 01 36.3
WLRG
FRII
3C444
N
E
Gemini/GMOS-S: median filtered image
5 GHz VLA radio map
Notes
This WLRG/FRII is at the centre of a cluster. In our Gemini GMOS-S image the galaxy appears surrounded by the diffuse halo typical of central cluster galaxies, and also shows hints of a broad fan or shells towards the NE (Ramos Almeida et al. 2011a). By looking at our processed images, we also detect a knotty sub-structure in the near-nuclear regions of the galaxy, which may be due to patchy dust obscuration. Evidence for a dust lane is also found in the model-subtracted NIR image of Inskip et al. (2010). The NIR data also reveal an excess of diffuse emission towards the east, coinciding with our tentative detection of a fan or a shell. This source is one of the three galaxies in our Gemini observation program with dust as the only feature with secure detection.
Despite the fact that it belongs to the class of weak-line radio galaxies, with no broad permitted lines detected in its optical spectrum, this FR II radio galaxy displays a substantial UV excess. A significant contribution from a young stellar population is suspected (Tadhunter et al. 2002).
Chandra observations of the hot X-ray emitting gas show clear evidence for cavities that have been hollowed out by the expanding radio jets and lobes (Croston et al. 2011).
PKS2211-17
Spectral energy distribution. The blue solid line is fitted to the data from 109 to 1010 Hz. Extrapolating this line from the radio to the infrared SED tests whether non-thermal synchrotron emission from the lobes can contaminate the Spitzer mid-infrared flux. In this case the lobes emission lies out of the Spitzer beam so cannot contaminate the Spitzer data. The weak, flat spectrum, non-thermal radio core emission is also not likely to contaminate the Spitzer infrared flux data for this object.