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 DataPKS1559+02_files/1559_70um.fits
Spitzer 160um DataPKS1559+02_files/1559_160um.fits


VLA 5GHzPKS1559+02_files/1559+02.ICL001.3

Spitzer IRS spectra



Morganti et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS1559+02_files/1559_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 objectPKS1602+01.html
Frequency       Flux      Units	                Reference                
5GHz	         2.87        Jy                       Morganti et al. (1993)
[OIII] λ5007     -13.30      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       15.2        mJy        	        Dicken et al. (2008)
22 GHz core      11.2        mJy	                 Dicken et al. (2008)
24 microns	242.0      mJy	                 Dicken et al. (2008)
70 microns	470.0      mJy	                 Dicken et al. (2008)
160 microns	262.8      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS1559+02_files/p1559.fits


16 02 27.38

+01 57 55.7





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

Inskip et al. (2010)



ISAAC K-band dataPKS1559+02_files/out_1559.fits


    The WFPC2/HST images of this NLRG/FRII source reveal a bifurcated dust lane structure extending ∼3 kpc to the NE of the galaxy nucleus, with the radio axis lying roughly perpendicular to the dust lanes. The nuclear structure, as revealed by the HST image, appears to be complex and possibly double (de Koff et al. 1996, 2000). The presence of a bright star close to the galaxy complicates its morphological classification. However, by looking at our processed Gemini GMOS-S images (unsharp-masked and especially smoothed galaxy-subtracted) the presence of dust lanes becomes clear. The galaxy nucleus appears double as well, but it is difficult to say whether is intrinsically double or just apparently divided by the dust lane. On larger scales the GMOS-S image reveals a system of sharply defined shells at radii of ∼16 and 30 kpc to the SE, and ∼14 and 22 kpc to the NW; these sharply defined shell features are reminiscent of the systems of shells detected around some elliptical galaxies in the nearby Universe by Malin & Carter (1983). We measure surface brightnesses of μ_V = 23.2 and 23.6 mag arcsec^−2 for the inner and outer shells, respectively. The larger of the shells to the SE was also detected by Heckman et al. (1986), while Inskip et al. (2010) detected the inner shell to the SE (16 kpc radial distance form the nucleus) in the near-infrared K-band, claiming that an elongated tidal feature appears to be connecting the galaxy nucleus with a satellite object to the south. Emission-line contamination can be ruled out, since strong emission lines do not fall in the r′ filter used for the observations.


Gemini GMOS-S Smooth galaxy subtracted image

Ramos Almeida et al. (2011a)

Gemini/GMOS-S: Unsharp mask 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)