Flux data

Available Data Downloads

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS0945+07_files/0945_70um.fits
Spitzer 160um DataPKS0945+07_files/0945_160um.fits


VLA 5GHzPKS0945+07_files/0945+07.ICL001.3

Spitzer IRS spectra



Morganti et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0945+07_files/0945_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 objectPKS1136-13.html
Frequency       Flux      Units	                Reference                
5GHz	         2.64        Jy                       Morganti et al. (1993)
[OIII] λ5007      -13.39      Log erg/cm2/s    Tadhunter et al. (1993)
15GHz core       13.9        mJy        	        Dicken et al. (2008)
22 GHz core      11.7        mJy	                 Dicken et al. (2008)
24 microns	47.7        mJy	                 Dicken et al. (2008)
70 microns	19.4        mJy	                 Dicken et al. (2008)
160 microns	<44.1      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS0945+07_files/p0945_add.fits


09 47 45.15

+07 25 20.4





    This BLRG/FRII was studied in detail by Prieto et al. (1993), who found spectacular extended emission-line structures. The optical morphology of this system was also studied by Heckman et al. (1986), and they reported the detection of several knots and tails which very likely correspond to line-emitting gas. The Gemini GMOS-S r’ optical image does not reveal any of these features, but it shows a shell of μ_V =24.4mag arcsec^−2  ∼7 kpc to the NW of the nucleus. In fact, emission-line contamination of the shell is not a serious issue because strong emission lines do not fall in the r′ filter employed in our observations. Indeed, this is confirmed by the presence of this shell in the K-band images of this galaxy (Inskip et al. 2010).

Gemini/GMOS-S: median filtered image

Images, Maps, Spectra and SEDs

    5 GHz VLA 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.  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)