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 DataPKS1306-09_files/1306_70um.fits
Spitzer 160um DataPKS1306-09_files/1306_160um.fits
VLA 5GHzPKS1306-09_files/1306-09.ICL001.5
ESO Optical spectraPKS1306-09_files/

Spitzer IRS spectra


PKS 1306-095 at 2291 MHz from the SHEVE array. The peak level is 0.30 Jy/beam and contours are shown at -5, 5, 10, 20, 40, 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 DataPKS1306-09_files/1306_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 objectPKS1318-43.html
Frequency       Flux      Units	                Reference                
5GHz	         1.9          Jy                       Morganti et al. (1993)
[OIII] λ5007      -14.79       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	4.6          mJy	                 Dicken et al. (2008)
70 microns	21.7        mJy	                 Dicken et al. (2008)
160 microns	<29.2      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1306-09_files/p1306_add.fits


13 08 39.17

-09 50 32.6





K-band (2.2 microns) image. 20x20 arcsecs.

Inskip et al. (2010)



SOFI K-band dataPKS1306-09_files/out_1306.fits


    The Gemini GMOS-S optical image reveals a secondary nucleus for this NLRG/CSS source (Ramos Almeida et al. 2011a), which is also detected in the residuals of the model-subtracted K-band image analysed by Inskip et al. (2010). The galaxy lies in a group of galaxies. From both the optical and NIR data, the radio galaxy is very likely undergoing interactions with other objects in the group. In addition to the double nucleus, we detect a sharply defined shell ∼20 kpc to SE of the radio galaxy, of surface brightness μ_V =24.5 mag arcsec^−2.

    This CSS radio galaxy has a large UV excess, only narrow emission lines, and significant UV polarization. Emission lines [OIII]5007, 4959 and H are detected, but the ionization state is only moderate. The information about the continuum is limited, but the Ca II H line is marginally detected. Details of the ionization and kinematics 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.

    Given that the polarization E-vector angle is closer to the parallel than the perpendicular to the radio axis, the polarization mechanism may not be anisotropic scattering, but some alternative mechanism such as dichroic absorption or synchrotron emission. The low level of intrinsic polarization suggests that if the polarization mechanism is anisotropic scattering, the scattered component does not dominate the UV excess (Tadhunter et al. 2002).

    Extrapolation of the radio spectrum suggests the non-thermal synchrotron radio lobe emission may contaminate the MFIR flux in this radio galaxy, because the lobes lie within the Spitzer beam (Dicken et al. 2008).

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 inside the Spitzer beam so non-thermal contamination is a possibility for the Spitzer data. However, the weak, flat spectrum, non-thermal radio core emission is not likely to contaminate the Spitzer infrared flux data for this object.

Dicken et al. (2008)