Flux data

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Images, Maps, Spectra and SEDs

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS1151-34_files/1151_70um.fits
Spitzer 160um DataPKS1151-34_files/1151_160um.fits
VLA 5GHzPKS1151-34_files/1151-348.ICL001.2
ESO Optical spectraPKS1151-34_files/

Spitzer IRS spectra


PKS 1151-348 at 2291 MHz from the SHEVE array. The peak level is 1.57 Jy/beam and contours are shown at -0.75, 0.75, 1.5, 3, 6, 12, 18, 35, 50, 65, 80% of the peak. ( Right) PKS 1151-348 at 8421 MHz from the SHEVE array. The peak level is 0.44 Jy/beam and contours are shown at -1.5, 1.5, 3, 6, 12, 18, 35, 50, 65, 80% of the peak.

Tziomis et al. (2002)


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS1151-34_files/1151_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 objectPKS1216+06.html
Frequency       Flux      Units	                Reference                
5GHz	         2.78        Jy                       Morganti et al. (1993)
[OIII] λ5007      -13.95      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	16.4        mJy	                 Dicken et al. (2008)
70 microns	51.5        mJy	                 Dicken et al. (2008)
160 microns	<46.3      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1151-34_files/p1151.fits


11 54 21.79

-35 05 29.1





    The presence of a young stellar population in this QSO/CSS is indicated by the low EW PAH feature detected in its Spitzer MIR spectrum (Dicken et al. 2011). The optical Gemini GMOS-S image reveals a spectacular extended structure for this system, with a prominent tidal tail/arc feature ∼34 kpc to the NW that connects to a compact secondary nucleus ∼27 kpc to the north of the quasar, as well as a broad fan of emission extending ∼38 kpc to the east of the nucleus. The overall morphology of the extended structure to the N-NW suggests that the quasar host galaxy is strongly interacting with a late-type spiral galaxy (possibly a barred spiral galaxy). Since the spiral structure of the interacting galaxy is reasonably coherent (although somewhat asymmetric), it appears that we are observing the system around the first pericentre passage of the interacting galaxies, rather than in the final stages of a merger as the nuclei coalesce. For this galaxy there are neither optical spectra nor infrared data suitable for assessing the degree of emission-line contamination of the detected features.

    The optical spectrum is characteristic of BLRG/Q: rich, high-ionization narrow-line spectrum, strong, highly structured Balmer lines, and a blue continuum.


Gemini GMOS-S Unsharp masked image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: median filtered image



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)