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X-Ray data
Spitzer IRS spectra
PKS0252-71
PKS 0252-712 at 2291 MHz from the SHEVE array. The peak level is 1.14 Jy/beam and contours are shown at -1.5, 1.5, 3, 6, 12, 24, 36, 48, 72, 96% of the peak.
PKS0252-71
Spitzer IRS spectra
Dicken et al. (in preperation)
PKS0252-71
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 1.58 Jy Morganti et al. (1993)[OIII] λ5007 -14.98 Log erg/cm2/s Tadhunter et al. (1993)
15GHz core - mJy Dicken et al. (2008)
22 GHz core - mJy Dicken et al. (2008)
24 microns 2.9 mJy Dicken et al. (2008)
70 microns 9.1 mJy Dicken et al. (2008)
160 microns 37.4 mJy Dicken et al. (2008)
X-ray - - -](PKS0252-71_files/shapeimage_17.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.566
02 52 46.28
-71 04 35.9
NLRG
CSS
-
Notes
Contamination of images and spectra by a foreground star preclude detailed study of the optical continuum in this NLRG/CSS radio galaxy. The optical spectrum shows high-ionization emission lines (Tadhunter et al. 1993). Details of the ionization and kinematics of the emission line gas in this source are discussed in Holt et al. (2008, MNRAS, 387, 639) and Holt et al. (2009, MNRAS, 400, 589) respectively.
In deep optical images PKS 0252−71 appears to be surrounded by an amorphous halo which points towards a fainter companion galaxy at ∼33 kpc to the south, thus indicating a possible interaction between the galaxies (Ramos Almeida et al. 2011a, Fig. B43). The images confirm that the bright object ∼3 arcsec to the SE of the radio galaxy host is a star. Unfortunately, the relatively poor seeing of this image (FWHM = 1 arcsec) prevents a clear detection of other possible signs of disturbance.
Gemini/GMOS-S: median filtered image
XMM
PKS0252-71
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.