Flux data
Available Data Downloads
Infrared data
Radio data
Optical data
X-Ray data
Chandra
Spitzer IRS spectra
PKS0945+07
Spitzer IRS spectra
Dicken et al. (in preperation)
PKS0945+07
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 2.64 Jy Morganti et al. (1993)
[OIII] λ5007 -13.39 Log erg/cm2/s Tadhunter et al. (1993)
15GHz core 13.9 mJy Dicken et al. (2008)
22 GHz core 11.7 mJy Dicken et al. (2008)
24 microns 47.7 mJy Dicken et al. (2008)
70 microns 19.4 mJy Dicken et al. (2008)
160 microns <44.1 mJy Dicken et al. (2008)
X-ray - - -](PKS0945+07_files/shapeimage_18.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.086
09 47 45.15
+07 25 20.4
BLRG
FRII
3C227
Notes
This BLRG/FRII was studied in detail by Prieto et al. (1993), who found spectacular extended emission-line structures. The optical morphology of this system was also studied by Heckman et al. (1986), and they reported the detection of several knots and tails which very likely correspond to line-emitting gas. The Gemini GMOS-S r’ optical image does not reveal any of these features, but it shows a shell of μ_V =24.4mag arcsec^−2 ∼7 kpc to the NW of the nucleus. In fact, emission-line contamination of the shell is not a serious issue because strong emission lines do not fall in the r′ filter employed in our observations. Indeed, this is confirmed by the presence of this shell in the K-band images of this galaxy (Inskip et al. 2010).
Gemini/GMOS-S: median filtered image
Images, Maps, Spectra and SEDs
5 GHz VLA radio map
PKS0945+07
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.