Flux data
Available Data Downloads
Infrared data
Radio data
Optical data
X-Ray data
Chandra
Spitzer IRS spectra
PKS0404+03
Spitzer IRS spectra
Dicken et al. (in preperation)
PKS0404+03
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.
![Wavelength/
Frequency Flux Units Reference
5GHz 2.39 Jy Morganti et al. (1993)
[OIII] λ5007 -14.42 Log erg/cm2/s Tadhunter et al. (1993) 15GHz core 19.8 mJy Dicken et al. (2008)
22 GHz core - mJy Dicken et al. (2008)
24 microns 30.8 mJy Dicken et al. (2008)
70 microns 70.9 mJy Dicken et al. (2008)
160 microns - mJy Dicken et al. (2008)
X-ray - - -](PKS0404+03_files/shapeimage_17.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.089
04 07 16.49
+03 42 25.8
NLRG
FRII
3C105
N
E
Notes
This galaxy has strong optical [O III] λλ5007, 4959 lines, as well as weak Hβ. Curiously [OII]λ3727 is not detected. This may indicate an unusually high ionization state or a large reddening. The continuum colours appear typical of early-type galaxies, although there are no clear detections of stellar continuum features.
The presence of a very bright star close (in projection) to this NLRG/FRII, along with the high Galactic dust extinction measured for this field (A_V > 1), means that optical observations of this source are less sensitive to low surface brightness features than for the other objects in the 2Jy sample. Nonetheless, processed optical Gemini images reveal hints of a faint shell towards the NE.
PKS 0404+03 has been previously studied in the optical by Zirbel (1996), and in the infrared by Donzelli et al. (2007) and Tremblay et al. (2007).
Gemini/GMOS-S: median filtered image
Images, Maps, Spectra and SEDs
6cm VLA radio map
PKS0404+03
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.
