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Spitzer IRS spectra
PKS0039-44
(Top) Image of 0039-44 at 3-cm (full resolution) with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 0.26 ratio). The contour levels are: , 1, 2, 4, 8, 16, 32, 64, 128, 256 mJy beam-1. The peak flux is 289.0 mJy beam-1. The synthesized beam of the observations is marked in the low left corner. The cross indicates the position (from di Serego et al. 1994) of the optical galaxy. (Bottom) Image of 0039-44 at 6-cm (Left) and 3-cm (Right) lower resolution with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 0.08 ratio for the 6 cm). The contour levels are: , 1, 2, 4, 8, 16, 32, 64, 128, 256 mJy beam-1. The peak flux at 6 cm is 587.8 mJy beam-1 and at 3 cm is 305.0 mJy beam-1
PKS0039-44
Spitzer IRS spectra
Dicken et al. (in preperation)
PKS0039-44
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 1.2 Jy Morganti et al. (1993)
[OIII] -13.55 Log erg/cm2/s Tadhunter et al. (1993)
15GHz core <1.1 mJy Dicken et al. (2008)
22 GHz core <0.9 mJy Dicken et al. (2008)
24 microns 33.0 mJy Dicken et al. (2008)
70 microns 68.7 mJy Dicken et al. (2008)
160 microns 84.6 mJy Dicken et al. (2008)
X-ray - - -](PKS0039-44_files/shapeimage_19.png)
Other name:
Redshift:
RA (j2000):
Dec (j2000):
Optical class:
Radio Class:
0.346
00 42 09.03
-44 14 01.3
NLRG
FRII
-
Notes
PKS 0039−44 is classified at optical wavelengths as an NLRG (Tadhunter et al. 1993, 1998); it has one of the largest emission line luminosities of all the intermediate redshift radio galaxies in the southern 2Jy sample (Tadhunter et al. 2002). Its FR II radio source is a relatively small, with its emission dominated by two lobes. No core or jets have been detected. Both lobes are polarized, with the eastern one showing a higher fractional polarization compared to the western side. The eastern lobe is slightly depolarized while the western side is consistent with no depolarization.
In the optical, this galaxy has a high ionization emission line spectrum with a strong blue, polarized continuum. PKS0039-44 has a large UV excess, significant UV polarization, but no broad permitted lines. Although the scattered AGN light is likely to be significant, with relatively low levels of intrinsic polarization, it is unlikely that this component dominates the UV continuum (Tadhunter et al. 2002).
The nucleus of this NLRG appears to be double in Gemini GMOS-S optical imaging (separation ∼4 kpc; Ramos-Almeida 2011a). Shell features are detected∼16kpc to the NW (μ_V =23.3mag arcsec−2), and ∼16 and∼27 kpc (μ_V =23.3 and 24.1 mag arcsec−2, respectively) to the SE of the nucleus. Although we do not consider it for the morphological classification of PKS 0039−44, our median filtered GMOS-S image shows a faint tail pointing to the star-like companion at ∼70 kpc to the west. This tentative tail appears co-aligned with the system of shells. Dust features also seem to be present in the galaxy nucleus. Emission-line contamination cannot be ruled out based on long-slit spectra in the case of the shells and the tail. However, our spectrum shows that the apparent secondary nucleus is likely to be dominated by [O III] λ5007 emission-line radiation.
Gemini/GMOS-S: median filtered image
3cm ATCA radio map
XMM
PKS0039-44
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.