Flux data

Available Data Downloads

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS0625-35_files/0625_35_70um.fits
Spitzer 160um DataPKS0625-35_files/0625_35_160um.fits


ESO Optical spectraPKS0625-35_files/

Spitzer IRS spectra




Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0625-35_files/0625_35_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 objectPKS0637-75.html
Frequency       Flux      Units	                Reference                
5GHz	         2.12	       Jy                       Morganti et al. (1993)
[OIII] λ5007      <-15.18    Log erg/cm2/s    Tadhunter et al. (1993)
15GHz core       571.6      mJy        	        Dicken et al. (2008)
22 GHz core      478.8      mJy	                 Dicken et al. (2008)
24 microns	 24.7	       mJy	                 Dicken et al. (2008)
70 microns	44.8         mJy	                 Dicken et al. (2008)
160 microns	131.0       mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:





K-band SOFI (2.2 microns) image. 40x40 arcsecs.

Inskip et al. (2010)



-35 29 16.3

06 27 6.65


SOFI K-band dataPKS0625-35_files/out_0625_35.fits

Gemini/GMOS-S: median filtered image


    Based on its relatively featureless optical continuum and strong core emission at optical and radio wavelengths, Wills et al. (2004) argue that PKS 0625−35 is a BL Lac. Our deep Gemin image of this low-redshift WLRG does not reveal any morphological peculiarity associated with a merger or interaction (Ramos Almeida et al. 2011a), but a one-sided jet pointing to the SE can be seen, which was also found by Inskip et al. (2010) in their residual NIR image. The detection of this jet supports the classification of this object as a BL-Lac by Wills et al. (2004).

    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 makes a substantial contribution to the MFIR flux in this radio galaxy (Dicken et al. 2008).


Gemini GMOS-S smooth galaxy subtracted image

Ramos Almeida et al. (2011a)

Gemini imagePKS0625-35_files/pks0625_35_stamp.fits

Images, Maps, Spectra and SEDs


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)

VLA 5GHzPKS0625-35_files/PKS0625.ICL001.6.fits