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 DataPKS1934-63_files/1938_70um.fits
Spitzer 160um DataPKS1934-63_files/1934_160um.fits


Spitzer IRS spectra


VLBI images of PKS 1934-638 at 2.3, 4.8 and 8.4 GHz (from Tzioumis et al. 1997). The top-right image is at a higher resolution because it includes Hartebeesthoek data. The other three images have approximately the same resolution of about 5 mas.

Tziomis et al. (2002)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS1934-63_files/1938_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 objectPKS1938-15.html
SOFI K-band dataPKS1934-63_files/out_1934.fits
Frequency       Flux      Units	                Reference                
5GHz	         6.45        Jy                       Morganti et al. (1993)
[OIII] λ5007     -14.00      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	17.4         mJy	                 Dicken et al. (2008)
70 microns	19.9         mJy	                 Dicken et al. (2008)
160 microns	<33.2       mJy	                 Dicken et al. (2008)
X-ray            	-	        -	         -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1934-63_files/p1934.fits


19 39 24.99

-63 42 45.6





K-band SOFI (2.2 microns) image. 30x30 arcsecs.

Inskip et al. (2010)




Gemini GMOS-S Unsharp masked image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: median filtered image


    This compact NLRG/GPS source is hosted in a double and highly disturbed system. The Gemini GMOS-S optical imaging shows two bright nuclei separated by ∼9 kpc, embedded in a common and irregular envelope. Two tidal tails extending towards the SW from the radio galaxy and to the north from its companion are detected with surface brightnesses of 23.1 and 23.4 mag arcsec^−2 , respectively. All the previous features were also detected by Heckman et al. (1986) with the same μ_V values. They observed the radio galaxy and companion in both B and V bands, reporting an integrated colour of B − V = 1.25, which is ∼0.3 mag bluer than the normal colour of elliptical galaxy at z = 0.2 (Fukugita et al. 1995). Although much of the blue light excess in this source is likely to be due to AGN-related continuum components such as scattered light and nebular continuum (see object-specific discussion in Tadhunter, Shaw & Morganti 1994; Tadhunter et al. 2002), evidence for on-going star formation activity in this source is provided by the detection of PAH emission features at MIR wavelengths by Dicken et al. (2011). Note that the optical tidal features described by Ramos Almeida et al. (2011a) are also reported in the K-band imaging study of Inskip et al. (2010), indicating their continuum-emitting nature. Our long-slit spectra also confirm that the companion galaxy and its associated tidal tail are dominated by continuum emission.

    As discussed in Tadhunter et al. (1994), this GPS radio galaxy is significantly polarized in the UV with the polarization E-vector close to perpendicular to the radio axis. No broad permitted lines are detected in our optical spectra. It is likely that scattered AGN light makes a significant contribution to the UV excess in this source.

In K-band near infrared image modeling, along with faint tidal features, our model residuals also show a third faint object lying just to the south of the interacting companion galaxy.

    Details of the kinematics and ionization of the emission line gas in this source are discussed in Holt et al. (2008, MNRAS, 387, 639) and Holt et al. (2009, MNRAS, 400, 589) respectively.


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)