Flux data

Available Data Downloads

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS0404+03_files/0404_70um.fits


ESO Optical spectraPKS0404+03_files/

Spitzer IRS spectra


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0404+03_files/0404_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)


VLA 6cm

baum et al. (1988)

Next objectPKS0405-12.html
Frequency       Flux      Units	                Reference                
5GHz	         2.39	       Jy                       Morganti et al. (1993)
[OIII] λ5007      -14.42      Log erg/cm2/s    Tadhunter et al. (1993) 15GHz core       19.8         mJy                	Dicken et al. (2008)
22 GHz core      -               mJy	                 Dicken et al. (2008)
24 microns	 30.8	        mJy	                 Dicken et al. (2008)
70 microns	70.9          mJy	                 Dicken et al. (2008)
160 microns	-                mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:


04 07 16.49

+03 42 25.8




Gemini imagePKS0404+03_files/p0404.fits


K-band SOFI (2.2 microns) image. 1x1 arcmin.

Inskip et al. (2010)



SOFI K-band dataPKS0404+03_files/out_0404.fits


    This galaxy has strong optical [O III] λλ5007, 4959 lines, as well as weak Hβ. Curiously [OII]λ3727 is not detected. This may indicate an unusually high ionization state or a large reddening. The continuum colours appear typical of early-type galaxies, although there are no clear detections of stellar continuum features.

    The presence of a very bright star close (in projection) to this NLRG/FRII, along with the high Galactic dust extinction measured for this field (A_V > 1), means that optical observations of this source are less sensitive to low surface brightness features than for the other objects in the 2Jy sample. Nonetheless, processed optical Gemini images reveal hints of a faint shell towards the NE.

    PKS 0404+03 has been previously studied in the optical by Zirbel (1996), and in the infrared by Donzelli et al. (2007) and Tremblay et al. (2007).

Gemini/GMOS-S: median filtered image

Images, Maps, Spectra and SEDs

    6cm 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)

VLA 5GHzPKS0404+03_files/0404+03.ICL001.6.fits