Flux data

Available Data Downloads

link to NED page

Infrared data

Radio data

Optical data

X-Ray data

Spitzer 70um DataPKS2221-02_files/2221_70um.fits



Spitzer IRS spectra

Spitzer 24um DataPKS2221-02_files/2221_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 objectPKS2243-12.html


Frequency       Flux      Units	                Reference                
5GHz	         2.28        Jy                        Morganti et al. (1993)
[OIII] λ5007      -12.76      Log erg/cm2/s     Tadhunter et al. (1993)
15GHz core       27.3        mJy                	Dicken et al. (2008)
22 GHz core      16.1        mJy	                 Dicken et al. (2008)
24 microns	232.1      mJy	                 Dicken et al. (2008)
70 microns	186.4      mJy	                 Dicken et al. (2008)
 X-ray            	-	        -	                 -

Other name:


RA (j2000):

Dec (j2000):

Optical class:

Radio Class:

Gemini imagePKS2221-02_files/p2221.fits


22 23 49.57

-02 08 12.4





K-band SOFI (2.2 microns) image. 35x35 arcsecs.

Inskip et al. (2010)



SOFI K-band dataPKS2221-02_files/out_2221.fits

Gemini/GMOS-S: median filtered image


Gemini GMOS-S Unsharp mask image

Ramos Almeida et al. (2011a)

Images, Maps, Spectra and SEDs


    This BLRG shows a very broad and asymmetric Hα profile in the optical spectrum first reported by Osterbrock, Koski & Phillips (1975). In the NIR, its morphology appears dominated by a nuclear point source, and the host galaxy is well reproduced by a de Vaucouleurs elliptical in both the NIR (Inskip et al. 2010) and the optical (Govoni et al. 2000). Our deep Gemini optical image reveals the spectacular morphology of this galaxy, which is clearly interacting with a close companion that appears obviously distorted in the direction of the radio galaxy host. The separation of the radio source and the companion galaxy is ∼37 kpc. The radio galaxy shows a broad fan of surface brightness μ_V = 25.6 mag arcsec^−2 towards the SW that is co-aligned with the axis of the double galaxy system, and a shell towards the east with μ_V =25.3 mag arcsec^−2. Long-slit spectra of this source (Tadhunter et al. 1986) demonstrate that the flux in the outer distorted structure is not dominated by emission lines.


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)