Flux data

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Images, Maps, Spectra and SEDs

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS2314+03_files/2314_70um.fits
Spitzer 160um DataPKS2314+03_files/2314_160um.fits
VLA 5GHzPKS2314+03_files/2314+03.ICL001.3
ESO Optical spectraPKS2314+03_files/

Spitzer IRS spectra


(Top) 5GHz

Morganti et al. (1993)

(Middle) Image of 2314+03 at 6-cm. The contour levels are: , 1, 2, 4, 8, 16, 32, 64, 128, 256 mJy beam-1. The peak flux is 400.7 mJy beam-1. (Bottom) Zoom-in of the eastern (Left) and of the western lobe (Right) of 2314+03 at 6-cm with superimposed vectors indicating the projected electric field direction. The vectors are proportional in length to the fractional polarisation (1 arcsec = 0.25 ratio for the eastern lobe and 1 arcsec = 0.5 ratio for the western lobe). The contour levels are: , 1, 2, 4, 8, 16, 32, 64, 128, 256, 512 mJy beam-1.

Morganti et al. (1999)


Optical spectrum taken with ESO telescopes.

Tadhunter et al. (1993)


Spitzer IRS spectra

Dicken et al. (in preperation)

Spitzer 24um DataPKS2314+03_files/2314_24um.fits


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)

Next objectPKS2345-16.html
Frequency       Flux      Units	                Reference                
5GHz	         1.33        Jy                        Morganti et al. (1993)
[OIII] λ5007     -14.01      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       <162.3    mJy        	        Dicken et al. (2008)
22 GHz core      <92.6      mJy	                 Dicken et al. (2008)
24 microns	49.9        mJy	                 Dicken et al. (2008)
70 microns	511.5      mJy	                 Dicken et al. (2008)
160 microns	490.4      mJy	                 Dicken et al. (2008)
X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS2314+03_files/p2314.fits


23 16 35.21

+04 05 18.2




Gemini/GMOS-S: median filtered image

    5 GHz VLA radio map



    PKS2314+03 has a relatively compact FRII structure that was studied in detail by Ulvestad (1985) and Thomasson et al. (2003). It is dominated by a strong, steep-spectrum radio core and two lobes. The eastern lobe is quite compact and much closer to the nucleus compared to the western one. A strong asymmetry in the polarisation can be seen between the two lobes with the eastern one much less polarised (only 2%) than the western one consistent with what was found by Ulvestad (1985).

    This NLRG shows strong evidence for a YSP at both optical (Miller 1981, Tadhunter et al. 2002, Wills et al. 2008) and MIR/FIR wavelengths (Dicken et al. 2009, 2011) and it is classified as ULIRG based on its FIR luminosity. In Gemini optical imaging it appears clearly disturbed. We detect two broad and symmetrical fans of  surface brightness μ_V = 23.6 (south) and 23.3 (east) mag arcsec^−2 , extending to a maximum distance of ∼33 kpc to the south of the nucleus, and giving an overall butterfly-like appearance. The southern fan shows some bright knots. Pointing to the north, we detect a faint tail in our processed images. Our VLT spectra demonstrate that the fan features are dominated by continuum rather than emission-line radiation.

    The optical/UV spectrum of this FR II radio galaxy is clearly dominated by the light of a young stellar population, with the Balmer break and higher Balmer and HeI absorption lines clearly detected (Wills et al. 2008). Detailed spectral synthesis modelling by Wills et al. (2008) demonstrated that a combination of young stellar populations with both young and intermediate ages (<0.1 Gyr and 0.2 – 1.2 Gyr) is required in order to provide an adequate fit to our deep VLT spectrum.

    Details of the kinematics and ionization of the emission line gas in this source are discussed in Holt et al. (2008, MNRAS, 387, 639) and Holt et al. (2009, MNRAS, 400, 589) respectively.


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)