IGR J21247+5058

Type	Redshift	Radio Counterpart			Infrared Counterpart
		R.A. (J2000)	Dec. (J2000)	References (position)	R.A. (J2000)	Dec. (J2000)	References (position)
Radio Galaxy AGN/Sey 1 Broad line FRII	0.020	4C 50.55 (GPSR 93.319+0.394, KR2, NRAO 659 or BG 2122+50)		Ribo et al. 2004 Atel 235	2MASS 21243932+5058259		Ribo et al. 2004 Atel 235
		21h24m39.3s (+/-0.1s)	+50d58'26" (+/-1")		21h24m39.32784s	+50d58'25.9284"
Published Papers		Masetti et al. 2004, A&A 426, L41 Pandey et al. 2006 A&A 446, 471 Bazzano et al. 2006, ApJ, 649, L9 Malizia et al. 2007, ApJ, 668,81 Molina et al. 2007 MNRAS, 382,937 Molina et al. 2008 MNRAS, 390, 1217 Winter et al. 2009, ApJ, 690, 1322 Tazaki et al. 2010, ApJ, 721, 1340

Miscellaneous :

NVSS contour plot here

2MASS K-band plot here

J=13.27, H=12.38, K=11.37. Optical counterpart with B=16.9 and R=15.1 (USNO B1 cat.)

Possible redshift z=0.02, equivalent to about 94 Mpc (Masetti et al. 2004)

Possible contamination by a superposition of a Galctic star (Masetti et al. 2004)

Bazzano et al. 2006 (ApJ):

Molina et al. 2007 (MNRAS):

Broad band analysis
Morphology of the (radio) source is typicalof edge-brightened FRII
Vewing angle theta=35deg
X-ray spectral analysis (XMM-Newton, INTEGRAL, and Swift)=> complex absorption due to two layers of material that cover partially the source with different covering fractions.
Spectrum shows the presence of a cut-off at ~75 keV.
Possible evolution in the source absorption related to flux variations.
To reconcile IGR J21247+5058 with being a Sey1: torus surrounding the source is not continuuous but clumpy

Tazaki et et al. 2010 :

80-ks Suzaku observation
Brightest broad-line radio galaxy in the hard X-ray sky (> 10 keV)
Broadband (1--60 keV) Suzaku-Swift spectrum : power law (Γ=1.65) high-energy cutoff (~ 105 keV), dual absorption layers (N_H1 ~ 7.9x10²² cm-2; N_H2 ~ 0.75x10²² cm-2 covering fraction f = 21%), + reflection component (solid angle: Ω/2π = 0.2)
Jets contribute a negligible amount to the total X-ray emission.
Thermal comptonization reveals a cold (kT ~ 31 keV) and optically-thick corona (τ ~ 3).
Narrow Fe-Kalpha emission line (EW ~ 19 eV) =>truncated disc and/or inner radius shielded by a comptonizing medium

Last updated 23 August 2010