PKS0105-16

Flux data

Available Data Downloads

Images, Maps, Spectra and SEDs

(definitions)Definitions.html
link to NED pagehttp://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=0105-16&extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS0105-16_files/0105_70um.fits
Spitzer 160um DataPKS0105-16_files/0105_160um.fits
VLA 5GHzPKS0105-16_files/0105-16.ICL001.3
ESO Optical spectraPKS0105-16_files/s0105.zip

Spitzer IRS spectra

PKS0105-16

5GHz map

Morganti et al. (1993)

PKS0105-16

Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)

PKS0105-16

Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS0105-16_files/0105_24um.fits

PKS0105-16

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.

Dicken et al. (2008)

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Wavelength/
Frequency       Flux      Units	                Reference                
5GHz	         1.17	       Jy                       Morganti et al. (1993)
[OIII]                -14.37        Log erg/cm2/s    Tadhunter et al. (1993) 15GHz core	<1.1         mJy    	        Dicken et al. (2008)
22 GHz core	<2.3         mJy	                 Dicken et al. (2008)
24 microns	9.7	       mJy	                 Dicken et al. (2008)
70 microns	<11.8       mJy	                 Dicken et al. (2008)
160 microns	<22.5       mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -http://adsabs.harvard.edu/abs/1993MNRAS.263.1023Mhttp://adsabs.harvard.edu/abs/1993MNRAS.263..999Thttp://adsabs.harvard.edu/abs/2008ApJ...678..712Dhttp://adsabs.harvard.edu/abs/2008ApJ...678..712Dhttp://adsabs.harvard.edu/abs/2008ApJ...678..712Dhttp://adsabs.harvard.edu/abs/2008ApJ...678..712Dhttp://adsabs.harvard.edu/abs/2008ApJ...678..712Dshapeimage_19_link_0shapeimage_19_link_1shapeimage_19_link_2shapeimage_19_link_3shapeimage_19_link_4shapeimage_19_link_5shapeimage_19_link_6

Other name:

Redshift:

RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

0.400

01 08 16.9

-16 04 20.6

NLRG

FRII

3C32

PKS0105-16

K-band SOFI (2.2 microns) image. 20x20 arcsecs.

Inskip et al. (2010)


N

E

Gemini imagePKS0105-16_files/p0105.fits
SOFI K-band dataPKS0105-16_files/out_0105.fits

Notes

    Gemini optical imaging of this NLRG/FRII galaxy reveals a bridge of μ_V = 24.6 mag arcsec−2 that appears to link the radio galaxy host with an early-type galaxy of similar brightness ∼70 kpc NW. Emission-line contamination of the detected feature cannot be ruled out based on the existing long-slit spectra (Ramos Almeida et al. 2011a).

    This FR II radio galaxy has a modest UV excess, no significant UV polarization, and no clear detection of broad permitted lines. The origin of its UV excess is not clear (Tadhunter et al. 2002).

PKS0105-16

Gemini GMOS-S Unsharp masked image

Ramos Almeida et al. (2011a)


Gemini/GMOS-S: median filtered image

x

    5 GHz VLA radio map

XMM

PKS0105-16

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.

Dicken et al. (2008)