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 DataPKS1602+01_files/1602_70um.fits
Spitzer 160um DataPKS1602+01_files/1602_160um.fits
VLA 5GHzPKS1602+01_files/1602+01.ICL001.2
ESO Optical spectraPKS1602+01_files/

Spitzer IRS spectra


(Top) 5Ghz

Morganti et al. (1993)

Image of 1602+01 at 6-cm. The contour levels are: , 1, 2, 3, 4, 6, 8, 10, 12, 14, 16, 20, 25, 30, 40, 50, 75, 100, 125 mJy beam-1. The peak flux is 94.5 mJy beam-1. Image of 1602+01 at 6-cm with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 0.5 ratio). The contour levels are: , 1, 2, 4, 8, 16, 32, 64 mJy beam-1. The peak flux is 94.5 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 DataPKS1602+01_files/1602_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 objectPKS1637-77.html
Frequency       Flux      Units	                Reference                
5GHz	         1.13        Jy                       Morganti et al. (1993)
[OIII] λ5007     -14.20      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       63.7        mJy        	        Dicken et al. (2008)
22 GHz core      65.5        mJy	                 Dicken et al. (2008)
24 microns	7.7          mJy	                 Dicken et al. (2008)
70 microns	12.3        mJy	                 Dicken et al. (2008)
160 microns	<32.4      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:


16 04 45.35

+01 17 50.8





    At radio wavelengths this source is dominated by a one sided knotty jet to the SE of the nucleus (Morganti et al. 1999). In terms of its high degree of curvature, this jet shows clear morphological similarities with PKS0035−02. Similarities are also present in the optical spectra of the two objects. In fact, in the optical PKS1602+01 has a high ionization emission line spectrum showing (as 0035−02)  broad components to the Balmer lines (Shaw et al. 1995; Tadhunter et al. 2002). The [OII] λ3727 and [OIII] λ5007 may be slightly extended.

    The Gemini GMOS-S optical image shows several signs of interaction. Towards the north of the galaxy nucleus we detect a bright and smooth fan of μ_V = 21.34 mag arcsec^−2 . On the opposite side there is a shell of μ_V = 23.3 mag arcsec^−2. In addition, and immersed in the shell envelope, we detect a sharp knot-like feature that extends up to 23 kpc and that is closely aligned (PA = 148 degrees) with the inner axis of the radio jet (PA = 145 degrees: see radio images in Morganti et al. 1999). At a distance of 18 kpc from the nucleus, the latter feature is close to, but does not exactly coincide with, the third knot in the radio jet leading to the south of the nucleus. The WFPC2/HST images of this galaxy only revealed an elliptical nucleus with a faint halo of emission surrounding it (de Koff et al. 1996). 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.

    Based on the extrapolation of the high frequency radio core component towards the infrared region of the spectral energy distribution, non-thermal core synchrotron emission may contaminate the MFIR flux in this radio galaxy (Dicken et al. 2008).

Gemini imagePKS1602+01_files/p1602.fits

Gemini/GMOS-S: median filtered image

    6cm 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.  However, extrapolating the, flat spectrum, radio core SED into the infrared, shows that the core synchrotron emission could be a possible source of non-thermal contamination to the thermal infrared flux.

Dicken et al. (2008)