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 DataPKS1136-13_files/1136_70um.fits
Spitzer 160um DataPKS1136-13_files/1136_160um.fits
VLA 5GHzPKS1136-13_files/1136-13.ICL001.4
ESO Optical spectraPKS1136-13_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 DataPKS1136-13_files/1136_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 objectPKS1151-34.html
Frequency       Flux      Units	                Reference                
5GHz	         1.9          Jy                       Morganti et al. (1993)
[OIII] λ5007      -13.39      Log erg/cm2/s    Tadhunter et al. (1993)
15GHz core       234.7      mJy        	        Dicken et al. (2008)
22 GHz core      230.4      mJy	                 Dicken et al. (2008)
24 microns	13.8        mJy	                 Dicken et al. (2008)
70 microns	23.9        mJy	                 Dicken et al. (2008)
160 microns	<23.2      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:


11 39 10.57

-13 50 43.1





    The Gemini GMOS-S image of this QSO/FRII at redshift z = 0.55 reveals the optical counterpart of a radio jet extending up to 60 kpc in the NW from the radio galaxy (Uchiyama et al. 2007). We also detect a shorter tidal tail pointing to the west of the nucleus, for which we measure a surface brightness of μ_V = 22.6 mag arcsec^−2. There are also signs of another tail SE of the nucleus. The lack of either optical long-slit spectra or infrared data suitable for assessing the degree of emission-line contamination of the detected features prevents us from confirming whether the extended structures are dominated by continuum radiation.

    The optical spectrum is typical of quasars: broad Balmer lines and rich, high-ionisation narrow-line spectrum, with a blue continuum.

    Extrapolation of the high frequency radio core component towards the infrared region of the spectral energy distribution, suggests that the non-thermal core synchrotron emission may contaminate the MFIR flux in this radio galaxy. In addition, further non-thermal contamination by the radio lobes within the Spitzer beam, may be present.

Gemini imagePKS1136-13_files/p1136.fits


Gemini GMOS-S Unsharp masked image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: median filtered image

    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 inside the Spitzer beam so non-thermal contamination is a possibility for the Spitzer data. In addition, extrapolating the, flat spectrum, radio core SED into the infrared, shows that the core synchrotron emission could be another possible source of non-thermal contamination to the thermal infrared flux.

Dicken et al. (2008)