Flux data

Available Data Downloads

Images, Maps, Spectra and SEDs

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS2356-61_files/2356_70um.fits
Spitzer 160um DataPKS2356-61_files/2356_160um.fits


Spitzer IRS spectra


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS2356-61_files/2356_24um.fits


Spitzer MIPS infrared photometric observations. Left to right: 24 microns, 70 microns and 160 microns (when available). FOV are 5x5 arcmins for 24 microns, 5x2.5 arcmins for 70 microns and 0.5x5 arcmins for 160 microns.

Dicken et al. (2008)

Frequency       Flux      Units	                Reference                
5GHz	         4.56        Jy                        Morganti et al. (1993)
[OIII] λ5007     -13.42      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       59.7        mJy        	        Dicken et al. (2008)
22 GHz core      63.8        mJy	                 Dicken et al. (2008)
24 microns	41.0        mJy	                 Dicken et al. (2008)
70 microns	74.7        mJy	                 Dicken et al. (2008)
160 microns      <35.4      mJy                     Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS2356-61_files/p2356.fits


23 59 04.50

-60 54 59.1





K-band ISAAC (2.2 microns) image. 50x50 arcsecs.

Inskip et al. (2010)



ISAAC K-band dataPKS2356-61_files/out_2356.fits


Gemini GMOS-S Unsharp mask image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: median filtered image


    The radio imaging of the source shows an FRII morphology with very compact hotspots and long bridges of emission extending back to the weak core. It is classified as a NLRG at optical wavelengths, on the basis of its strong, high ionization emission line spectrum

    The optical morphology revealed by our deep Gemini/GMOS-S image shows a range of features that are very likely the result of a past merger/interaction. On smaller scales, we detect one arc-like irregular feature of surface brightness 24.9 mag arcsec^−2 in the V-band to the north  of the galaxy centre. There is also a shell towards the south of the galaxy, and a fainter one to the NE (μ_V =25.1 and 25.6 mag arcsec^−2, respectively). Further from the brighter shell there is also a broad fan/shell in the same direction, at a 25.8 mag arcsec−2 surface brightness level. Finally, at ∼82 and 118 kpc distance from the galaxy centre, there are two faint arcs towards the NW and SW, respectively. Note that the shell features detected in this galaxy are more irregular in appearance than the sharp shells detected in other objects in the 2Jy sample (e.g. PKS 1559+02 and PKS 0442−28) and in the nearby ellipticals studied by Malin & Carter (1983). Emission-line contamination is not a serious issue in the case of this galaxy because strong emission lines do not fall in the r′ filter employed in our observations.


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)