Flux data

Available Data Downloads

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS0620-52_files/0620_70um.fits
Spitzer 160um DataPKS0620-52_files/0620_160um.fits


ESO Optical spectraPKS0620-52_files/

Spitzer IRS spectra



Morganti et al. (1993)


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0620-52_files/0620_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)

Next objectPKS0625-53.html
Frequency       Flux      Units	                Reference                
5GHz	         1.25	       Jy                       Morganti et al. (1993)
[OIII] λ5007     -13.99       Log erg/cm2/s    Tadhunter et al. (1993)
15GHz core       118.6      mJy                	Dicken et al. (2008)
22 GHz core      101.2      mJy	                 Dicken et al. (2008)
24 microns	 4.5	       mJy	                 Dicken et al. (2008)
70 microns	47.3         mJy	                 Dicken et al. (2008)
160 microns	<24.3       mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS0620-52_files/p0652.fits


06 21 43.29

-52 41 33.3




Gemini/GMOS-S: median filtered image


    The deep r′ image for PKS0620-52 presented in Ramos Almeida et al. (2010a) suggests that this FRI radio galaxy is the dominant cD galaxy in a rich cluster, a conclusion supported by the presence of a moderately luminous X-ray halo (Siebert et al. 1996; Trussoni et al. 1999). However, in this case there is no clear evidence for morphological disturbance, apart from the high incidence of nearby companion galaxies that is expected at the centre of a galaxy cluster. Spectral synthesis modelling by Wills et al. (2004) shows clear evidence for a young stellar population, although the relatively narrow spectral coverage and low S/N of their spectra precluded the determination of an accurate age for the YSP. We have attempted to improve the determination of the properties of the YSP in this source by modelling a deeper, wider spectral coverage spectrum that was taken using the ESO 3.6-m telescope in 2007 (Tadhunter et al. 2011). We find that we can obtain good fits to both the continuum SED and the detailed absorption line features for YSP ages <0.9 Gyr and reddening in the range 0 < E(B − V) < 1.5mag; older YSP ages are ruled out because they over-predict the strengths of the Ca II H+K absorption line features. It is not possible to determine the ages and reddening of the YSP more accurately for PKS0620-52 with the existing data, since the YSP make a relatively small contribution to the optical continuum (10–25 per cent at 4720 A), although larger than in the case of Fornax A.

    Based on the extrapolation of the high frequency radio core component towards the infrared region of the spectral energy distribution, it is possible that the non-thermal core synchrotron emission may contaminate the thermal infrared flux in this radio galaxy Dicken et al. 2008).

Images, Maps, Spectra and SEDs

    5 GHz ATCA radio map



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.  However, extrapolating the, flat spectrum, radio core SED into the infrared, shows that the core synchrotron emission could be a possible source of non-thermal contamination to the thermal infrared flux.

Dicken et al. (2008)