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 DataPKS0806-10_files/0806_70um.fits
Spitzer 160um DataPKS0806-10_files/0806_160um.fits


VLA 5GHzPKS0806-10_files/0806_1993.fits

ESO Optical spectra

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 DataPKS0806-10_files/0806_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 objectPKS0842-75.html
Frequency       Flux      Units	                Reference                
5GHz	         1.63	      Jy                       Morganti et al. (1993)
[OIII] λ5007     -12.82      Log erg/cm2/s    Tadhunter et al. (1993)
15GHz core       32.7        mJy                	Dicken et al. (2008)
22 GHz core      20.7        mJy	                 Dicken et al. (2008)
24 microns	258.3     mJy	                 Dicken et al. (2008)
70 microns	489.7      mJy	                 Dicken et al. (2008)
160 microns	308.7      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS0806-10_files/p0810.fits


06 26 20.44

-53 41 35.2





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

Inskip et al. (2010)



SOFI K-band dataPKS0806-10_files/out_0806.fits


    The GMOS-S image of this NLRG/FRII shows a clearly disturbed morphology, including features such as a broad fan towards the east (μ_V = 23.4 mag arcsec^−2), a bright shell to NW and a fainter shell towards the west (μ_V = 23.3 and 24.6 mag arc- sec^−2, respectively: Ramos Almeida et al. 2011a). The unsharp-masked image also shows several bright knots of emission closer to the galaxy centre. Emission-line contamination of the features is not a serious issue here because strong emission lines do not fall in the r′-band filter employed in our observations. Inskip et al. (2010) also report the detection of the NW shell (or arc-like feature) in their K-band images. It is possible that the host galaxy is interacting with a smaller, extended companion object to the east.

    The optical spectrum shows a rich, high ionization emission-line spectrum. The optical emission lines are clearly extended in this object. Although the optical continuum spectrum does not require a young stellar population (any UV excess can be explained in terms of AGN-related continuum components), a low EW PAH feature is detected in the Spitzer IRS spectrum (Dicken et al. 2011).

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 out of the Spitzer beam so cannot contaminate the Spitzer data.  The, 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)