Flux data
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Infrared data
Radio data
Optical data
X-Ray data
Chandra
Spitzer IRS spectra
PKS0625-53
(Left) Image of 0625-53 at 6-cm with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 0.07 ratio). The contour levels are: , 1, 2, 3, 4, 6,8 mJy beam-1. The peak flux is 22.0 mJy beam-1. (Right) Image of 0625-53 at 6-cm with superimposed boxes proportional to the rotation measure (RM, 1 arcsec = 543 rad m-2). Filled squares represent positive numbers for the RM while empty squares represent negative numbers
PKS0625-53
Spitzer IRS spectra
Dicken et al. (in preperation)
PKS0625-53
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 1.85 Jy Morganti et al. (1993)
[OIII] λ5007 <-15.46 Log erg/cm2/s Tadhunter et al. (1993)
15GHz core 20.4 mJy Dicken et al. (2008)
22 GHz core 19.3 mJy Dicken et al. (2008)
24 microns 1.7 mJy Dicken et al. (2008)
70 microns <10.8 mJy Dicken et al. (2008)
160 microns <52.6 mJy Dicken et al. (2008)
X-ray - - -](PKS0625-53_files/shapeimage_18.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.054
06 26 20.44
-53 41 35.2
WLRG
FRI
-
N
E
Notes
This is a FRI galaxy associated with a dumbbell galaxy (Lilly & Prestage 1987; Gregorini et al. 1994) that is also the brightest member of the cluster Abell 3391. At the resolution of the 6cm observations, it shows a wide-angle tail structure with two tails sharply bending at about 20 arcsec north and 40 arcsec south of the nucleus. This morphology is also confirmed by the 13-cm ATCA image presented by Otani et al. (1998). From an X-ray/radio comparison, the latter authors found evidence for a possibly strong interaction between the radio jets and the surrounding material. The jets are deflected possibly as the result of pressure gradients or winds in the intracluster medium, and they seem to "escape'' into regions of lower X-ray brightness. This galaxy has also been observed at lower resolution by Gregorini et al. (1994). In their image, the northern tail is even more prominent and a low-brightness diffuse region is also observed as a western extension to the southern lobe.
The optical spectrum shows no emission lines and the continuum spectrum is typical of quiescent elliptical galaxies.
Our deep Gemini optical image shows a broad bridge linking the two galaxies, which are separated by a distance of ∼19 kpc, have highly distorted isophotes and are clearly interacting (Ramos Almeida et al. 2011a). The same morphology is found in the NIR images analysed in Inskip et al. (2010), who did not detect strong nuclear point source component in either object. Also noticeable in the Gemini GMOS-S image is the degree of distortion in the two galaxy companions located to the NW of the dumbbell system.
Extrapolation of the high frequency radio core component towards the infrared region of the spectral energy distribution suggests that the non-thermal core synchrotron emission may contaminate the MFIR flux in this radio galaxy (Dicken et al. 2008).
Gemini/GMOS-S: Unsharp mask image
Images, Maps, Spectra and SEDs
6 cm ATCA radio map
PKS0625-53
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.