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PKS2356-61
PKS2356-61
Spitzer IRS spectra
Dicken et al. (in preperation)
PKS2356-61
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 4.56 Jy Morganti et al. (1993)
[OIII] λ5007 -13.42 Log erg/cm2/s Tadhunter et al. (1993)
15GHz core 59.7 mJy Dicken et al. (2008)
22 GHz core 63.8 mJy Dicken et al. (2008)
24 microns 41.0 mJy Dicken et al. (2008)
70 microns 74.7 mJy Dicken et al. (2008)
160 microns <35.4 mJy Dicken et al. (2008)
X-ray - - -](PKS2356-61_files/shapeimage_17.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.096
23 59 04.50
-60 54 59.1
NLRG
FRII
-
N
E
Gemini/GMOS-S: median filtered image
Notes
The radio imaging of the source shows an FRII morphology with very compact hotspots and long bridges of emission extending back to the weak core. It is classified as a NLRG at optical wavelengths, on the basis of its strong, high ionization emission line spectrum
The optical morphology revealed by our deep Gemini/GMOS-S image shows a range of features that are very likely the result of a past merger/interaction. On smaller scales, we detect one arc-like irregular feature of surface brightness 24.9 mag arcsec^−2 in the V-band to the north of the galaxy centre. There is also a shell towards the south of the galaxy, and a fainter one to the NE (μ_V =25.1 and 25.6 mag arcsec^−2, respectively). Further from the brighter shell there is also a broad fan/shell in the same direction, at a 25.8 mag arcsec−2 surface brightness level. Finally, at ∼82 and 118 kpc distance from the galaxy centre, there are two faint arcs towards the NW and SW, respectively. Note that the shell features detected in this galaxy are more irregular in appearance than the sharp shells detected in other objects in the 2Jy sample (e.g. PKS 1559+02 and PKS 0442−28) and in the nearby ellipticals studied by Malin & Carter (1983). Emission-line contamination is not a serious issue in the case of this galaxy because strong emission lines do not fall in the r′ filter employed in our observations.
PKS2356-61
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.