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PKS2221-02
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.
PKS2221-02
![Wavelength/
Frequency Flux Units Reference
5GHz 2.28 Jy Morganti et al. (1993)
[OIII] λ5007 -12.76 Log erg/cm2/s Tadhunter et al. (1993)
15GHz core 27.3 mJy Dicken et al. (2008)
22 GHz core 16.1 mJy Dicken et al. (2008)
24 microns 232.1 mJy Dicken et al. (2008)
70 microns 186.4 mJy Dicken et al. (2008)
X-ray - - -](PKS2221-02_files/shapeimage_17.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.057
22 23 49.57
-02 08 12.4
BLRG
FRII
3C445
N
E
Gemini/GMOS-S: median filtered image
Images, Maps, Spectra and SEDs
Notes
This BLRG shows a very broad and asymmetric Hα profile in the optical spectrum first reported by Osterbrock, Koski & Phillips (1975). In the NIR, its morphology appears dominated by a nuclear point source, and the host galaxy is well reproduced by a de Vaucouleurs elliptical in both the NIR (Inskip et al. 2010) and the optical (Govoni et al. 2000). Our deep Gemini optical image reveals the spectacular morphology of this galaxy, which is clearly interacting with a close companion that appears obviously distorted in the direction of the radio galaxy host. The separation of the radio source and the companion galaxy is ∼37 kpc. The radio galaxy shows a broad fan of surface brightness μ_V = 25.6 mag arcsec^−2 towards the SW that is co-aligned with the axis of the double galaxy system, and a shell towards the east with μ_V =25.3 mag arcsec^−2. Long-slit spectra of this source (Tadhunter et al. 1986) demonstrate that the flux in the outer distorted structure is not dominated by emission lines.
PKS2221-02
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.