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 DataPKS1733-56_files/1733_70um.fits
Spitzer 160um DataPKS1733-56_files/1733_160um.fits


ESO Optical spectraPKS1733-56_files/

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 DataPKS1733-56_files/1733_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 objectPKS1814-63.html
ISAAC K-band dataPKS1733-56_files/out_1733.fits
Frequency       Flux      Units	                Reference                
5GHz	         3.37        Jy                       Morganti et al. (1993)
[OIII] λ5007     -13.69      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       293.6      mJy        	        Dicken et al. (2008)
22 GHz core      269.4      mJy	                 Dicken et al. (2008)
24 microns	29.2        mJy	                 Dicken et al. (2008)
70 microns	151.0      mJy	                 Dicken et al. (2008)
160 microns	318.2      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	         -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1733-56_files/p1733_add.fits


17 37 35.80

-56 34 03.4





K-band ISAAC (2.2 microns) image. 50x50 arcsecs.

Inskip et al. (2010)




    This BLRG/FRII, with evidence for starburst activity provided by its FIR excess and strong PAH features in its MIR spectrum (Dicken et al. 2009, 2010), lies in a relatively crowded field. Its optical morphology, as revealed by our Gemini GMOS-S image, is highly disturbed, showing at least two tidal tails: a shorter one pointing to the west and a longer one to the SE both having μ_V = 23.6 mag arcsec^−2. We also detect several arc-like irregular features, including a smooth, inner one (of μ_V = 23.6 mag arcsec^−2 ) up to 6.5 kpc in the SE direction and a larger one of μ_V = 24 mag arcsec^−2 extended up to 11.6 kpc to the NW. It is likely that at least part of the complex structure visible in the central regions of the galaxy is due to obscuration by a complex system of dust lanes. The brightest inner arc-like irregular structure is detected in the K-band, model-subtracted images presented by Inskip et al. (2010), who also suggest that the residuals from the subtraction display an excess of emission aligned with the major axis of the galaxy. In the outermost part of the radio galaxy host we also detect an interlocking series of fainter shells that extend to a maximum radius of ∼25 kpc to the SE and ∼17 kpc to the south. We measure surface brightnesses of μ_V = 24.4 and 24.0 mag arcsec^−2 for these outer shells, respectively. Emission-line contamination is not a serious issue in our GMOS-S image, since strong emission lines do not fall in the r′-band filter used for the observations. Based on integral-field spectroscopic observations, Bryant & Hunstead (2002) found evidence for a disturbed morphology, disrupted gas rotation and patchy starburst emission for this source. They claimed that the most plausible explanation for all of these features is an interaction or merger with an SE companion from which the radio galaxy would be accreting gas, but they did not find such a merging galaxy in the DSS-II and SuperCOSMOS images; our deeper GMOS-S image does not show any secondary nucleus.

    Note that the BLRG classification of this object is based on the detection of a broad Hα line in its optical spectrum (Hunstead et al. 1982, PASAu, 4, 447; Simpson et al. (1996, MNRAS,  281, 509).


Gemini GMOS-S median filtered 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)