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 DataPKS1355-41_files/1355_70um.fits
Spitzer 160um DataPKS1355-41_files/1355_160um.fits
ESO Optical spectraPKS1355-41_files/

Spitzer IRS spectra


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS1355-41_files/1355_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 objectPKS1510-08.html
Frequency       Flux      Units	                Reference                
5GHz	         1.44        Jy                       Morganti et al. (1993)
[OIII] λ5007      -13.70      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       102.7      mJy        	        Dicken et al. (2008)
22 GHz core      89.6        mJy	                 Dicken et al. (2008)
24 microns	53.1        mJy	                 Dicken et al. (2008)
70 microns	66.3        mJy	                 Dicken et al. (2008)
160 microns	<55.9      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1355-41_files/p1355.fits


13 59 00.23

-41 52 54.1





    The Gemini observations of this QSO at redshift z = 0.31 has the best seeing among all the GMOS-S observations of the 2Jy sample  (FWHM ∼ 0.4 arcsec). This fact is clearly reflected in the high quality of the images and the level of detail of the identified features. There is a sharp shell feature ∼24 kpc to the SE of the quasar and covering an angle of ∼60 degrees, along with a bright and narrow tail extending up to ∼22 kpc to the SE along PA = 121 degrees and pointing towards the arc. Although the latter feature is closely aligned with the axis of the large-scale radio structure (PA = 125 degrees), the high-frequency radio map presented in Dicken et al. (2008) shows no sign of any radio emission from the tail that might suggest that it is non-thermal in nature. For this galaxy, there are neither optical long-slit spectra nor infrared data suitable for assessing the degree of emission-line contamination of the detected features.

    The optical spectrum shows the quasar: strong, broad Balmer lines, blue continuum and [OIII]λλ5007, 4959 lines of moderate strength.


Gemini GMOS-S Unsharp masked image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: median filtered 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)