Flux data

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Images, Maps, Spectra and SEDs

link to NED page

Infrared data

Radio data

Optical data

X-Ray data


VLA 5GHzPKS2211-17_files/2211-ABC.ICL001.3
ESO Optical spectraPKS2211-17_files/



Morganti et al. (1993)


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)

Spitzer 24um DataPKS2211-17_files/2211_24um.fits
Next objectPKS2221-02.html
Frequency       Flux      Units	                Reference                
5GHz	         2.14        Jy                        Morganti et al. (1993)
[OIII] λ5007     -15.44      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       <1.3        mJy        	        Dicken et al. (2008)
22 GHz core      <1.8        mJy	                 Dicken et al. (2008)
24 microns	0.5          mJy	                 Dicken et al. (2008)
70 microns	<9.4        mJy	                 Dicken et al. (2008)
-                    	-              -                           -
X-ray            	-	        -	          -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS2211-17_files/p2211.fits


22 14 25.78

-17 01 36.3





K-band ISAAC (2.2 microns) image. 35x35 arcsecs.

Inskip et al. (2010)



ISAAC K-band dataPKS2211-17_files/out_2211.fits

Gemini/GMOS-S: median filtered image

    5 GHz VLA radio map


    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).


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.

Dicken et al. (2008)