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 DataPKS0347+05_files/0347_70um.fits
Spitzer 160um DataPKS0347+05_files/0347_160um.fits
VLA 5GHzPKS0347+05_files/0347+05.ICL001.2

Spitzer IRS spectra



Morganti et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0347+05_files/0347_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 objectPKS0349-27.html
Frequency       Flux      Units	                Reference                
5GHz	         1.26	       Jy                       Morganti et al. (1993)
[OIII] λ5007        -             Log erg/cm2/s    Tadhunter et al. (1993) 15GHz core       <2.2        mJy                	Dicken et al. (2008)
22 GHz core      <2.5        mJy	                 Dicken et al. (2008)
24 microns	 3.5	       mJy	                 Dicken et al. (2008)
70 microns	 30.8        mJy	                 Dicken et al. (2008)
160 microns	<52.2       mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:


03 49 50

+05 51 42.3




Gemini imagePKS0347+05_files/p0347.fits

UFTI K-band data


    The WLRG/FRII PKS 0347+05 is part of a spectacular interacting system, which includes a QSO/Seyfert 1 nucleus ∼26 kpc to the SW of the radio galaxy host itself (Ramos Almeida et al. 2011a, Tadhunter et al. 2011, in preparation). This object provides some of the best evidence for the triggering of radio/AGN activity as a result of a galaxy interaction in the 2Jy sample. In addition, Spitzer MIR and FIR data reveal the presence of a YSP, based on the detection of a FIR excess (Dicken et al. 2009) and strong PAH features (Dicken et al. 2011). The Gemini GMOS-S optical image shows a bridge linking the two interacting galaxies, and at least three tidal tails extending to the SW of the system. The closest tail to the QSO is the brightest, presenting a bright knot at the closest edge. The presence of dust features close to the radio galaxy is also clear, and consistent with a star-forming region. Long-slit spectra of the galaxy show that emission-line contamination is not a serious issue for most of the peculiar features detected in this system.

    This object is one of the most distant and radio luminous WLRG known.


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 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)