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 DataPKS1547-79_files/1547_70um.fits
Spitzer 160um DataPKS1547-79_files/1547_160um.fits
ESO Optical spectraPKS1547-79_files/

Spitzer IRS spectra


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS1547-79_files/1547_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)



Burgess et al. (2006)

Next objectPKS1549-79.html
Frequency       Flux      Units	                Reference                
5GHz	         1.38        Jy                       Morganti et al. (1993)
[OIII] λ5007     -13.68      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       -              mJy        	        Dicken et al. (2008)
22 GHz core      -              mJy	                 Dicken et al. (2008)
24 microns	7.9          mJy	                 Dicken et al. (2008)
70 microns	19.2        mJy	                 Dicken et al. (2008)
160 microns	<50.2      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1547-79_files/p1547_add.fits


15 55 21.6

-79 40 36.3





This BLRG/FRII is classified  as a double nucleus system, since the radio source has a fainter companion ∼9 kpc to the south of the nucleus, as revealed by our Gemini GMOS-S image. In addition, the GMOS-S optical image reveals a tidal tail extending ∼27 kpc to the NE of the galaxy centre of surface brightness μ_V = 24.3 mag arcsec^−2. In both the optical and the NIR, PKS 1547−79 appears as a clear interacting system, surrounded by several diffuse companions. Note that the companion galaxy ∼46 kpc to the west of the radio galaxy host has weak emission lines that suggest a similar redshift to PKS 1547−79. On the other hand, the much brighter early-type galaxy ∼70 kpc to the east, which also shows some signs of morphological disturbance, is at a much lower redshift. The continuum-emitting nature of the tidal tail of PKS 1547−79 cannot be either confirmed or discarded based on existing long-slit spectra (Tadhunter et al. 1998), but the secondary nucleus is detected in the NIR (Inskip et al. 2010).

The continuum properties of PKS1547-79 have been extensively discussed in Shaw et al. (1995), who argue that at least some of the significant UV polarization measured in this source may be caused by dichroic absorption in our Galaxy. Differential diffraction effects preclude detailed modelling of its continuum, but it is likely that the UV excess in this object is dominated by direct AGN light.

Interestingly, in the near-IR K-band image, this source is surrounded by a large number of faint features that are not duplicated elsewhere in the field, and are plausibly satellite systems.

The optical spectrum reveals high-ionization emission lines as well as broad wings to the Hß line. There are no detections of stellar absorption features.


Gemini GMOS-S Smooth galaxy subtracted image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: Unsharp mask image

    5 GHz ATCA 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)