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 DataPKS0442-28_files/0442_70um.fits
Spitzer 160um DataPKS0442-28_files/0442_160um.fits


VLA 5 GHz PKS0442-28_files/0442-28.ICL001.9

ESO Optical spectra

Spitzer IRS spectra


(Top) 5GHz

Morganti et al. (1993)

(Middle) Image of 0442-28 at 6-cm. The contour levels are: , 1, 2, 3, 4, 6, 8, 10, 15, 20, 25, 30, 50, 100, 200, 400 mJy beam-1. The peak flux is 197.0 mJy beam-1. (Bottom) Zoom-in of the southern (Right) and of the northern lobe (Left) of 0442-28 at 6-cm. with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 1.0 ratio). The contour levels are: , 1, 2, 4, 8, 10, 15, 20, 25, 30, 40, 50 mJy beam-1

Morganti et al. (1999)


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0442-28_files/0442_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 objectPKS0453-20.html
Frequency       Flux      Units	                Reference                
5GHz	         2.21	       Jy                       Morganti et al. (1993)
[OIII] λ5007     -13.96       Log erg/cm2/s    Tadhunter et al. (1993)
15GHz core      19.1         mJy                	Dicken et al. (2008)
22 GHz core      20.4        mJy	                 Dicken et al. (2008)
24 microns	 22.0	       mJy	                 Dicken et al. (2008)
70 microns	31.0         mJy	                 Dicken et al. (2008)
160 microns	<25.9       mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:


04 44 37.67

-28 09 54.6




Gemini imagePKS0442-28_files/p0442.fits


K-band SOFI (2.2 microns) image. 40x40 arcsecs.

Inskip et al. (2010)



SOFI K-band dataPKS0442-28_files/out_0442.fits


    The radio observations for this NLRG/FRII galaxy (Morganti et al. 1999) shows a complex morphology for its radio lobes. A core has been detected but no radio jets.

    This object has strong, narrow optical emission lines [O III] λλ5007, 4959 and [O II] λ3727 (Tadhunter et al. 1993). The optical continuum colours may be slightly bluer than those of typical early type-galaxies and there are no clear detections of stellar absorption features.  It is also detected in X-rays (Siebert et al. 1996), where it appears to be extended, even though this source is not known to be associated with a cluster.

    The optical image shows a faint, but sharply defined shell ∼50 kpc to SW of its nucleus in our GMOS-S image (Ramos Almeida et al. 2011a). This shell has a surface brightness μ_V = 25.7 mag arcsec^−2. There are several galaxies within ∼20 arcsec, any of them possibly interacting with the radio galaxy.


Gemini GMOS-S Unsharp masked image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: median filtered image

    5 GHz VLA 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)