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PKS1648+05
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 12.74 Jy Morganti et al. (1993)
[OIII] λ5007 -15.26 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 2.0 mJy Dicken et al. (2008)
70 microns <18.8 mJy Dicken et al. (2008)
160 microns 134.3 mJy Dicken et al. (2008)
X-ray - - -](PKS1648+05_files/shapeimage_18.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.154
16 51 08.16
+04 59 33.8
WLRG
FRI/FRII
Hercules A
Notes
PKS1648+05 (Her A) is a very well known unusual radio galaxy (with a morphology between FRI and FR II) studied in detail by Dreher and Feigelson (1984). This WLRG source is at the centre of a cooling flow cluster of galaxies at z = 0.154. A recent analysis of Chandra X-ray data showed that the cluster has cavities and a shock front associated with the radio source (Nulsen et al. 2005). Heckman et al. (1986) did not report the existence of any features for this galaxy from their optical imaging. However, our Gemini data reveal patchy dust features crossing the galaxy nucleus in a roughly east–west direction, out to a radius of ∼6.5 kpc to the east (Ramos Almeida et al. 2011a). Note that de Koff et al. (1996) and Baum et al. (1996) have used the HST to detect fine dust features in the nuclear regions of this galaxy, and they claim that the dust is distributed as two interlocking rings. Unfortunately, our Gemini observations do not have sufficient spatial resolution to allow us to confirm the ring-like morphology of the near-nuclear dust.
The optical spectrum shows two diffuse continuum components separated by 3 arcsec. Weak [OIII]λ5007 and moderate [OII]λ3727 lines are detected. Both components show an absorption line spectrum typical of early-type galaxies. The [OII] Emission is extended.
This powerful radio source has a small UV excess. The cause of the apparent UV excess is unknown (Tadhunter et al. 2002).
Gemini/GMOS-S: Unsharp mask image
PKS1648+05
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.