Swift/XRT follow-up of the unidentified INTEGRAL source IGR J03564+6242
ATel #4025; M. Molina, R. Landi (INAF/IASF Bologna), A. Bazzano, M. Fiocchi (INAF/IASF Rome), A. J Bird, S. P. Drave (Univ. Southampton)
on 10 Apr 2012; 09:08 UT
Credential Certification: Manuela Molina (email@example.com)
Subjects: Radio, X-ray, Gamma Ray, AGN, Blazar, Quasar
We report the possible association of the unidentified INTEGRAL source
IGR J03564+6242 with the radio galaxy 4C 62.08, obtained through
a Swift/XRT Target of Opportunity follow-up observation.
IGR J03564+6242 is listed in the 4th INTEGRAL/IBIS catalogue (Bird et al. 2010),
at coordinates RA (J2000) = 59.099 and Dec (J2000) = 62.714, with a positional uncertainty
of 4.6 arcmin. The source is flagged as Y
in the catalogue, indicating that it is mildly variable; the peak flux in the 20-40 keV band of
11.35ÃÂ±3.08X10-12 erg cm-2s-1.
The XRT observed the source four times between April 2, 2011 and April
10, 2011. The combined images reveal one X-ray source at 4.4 sigma confidence level
located at 5.4 arcminutes from the unidentified INTEGRAL source, i.e.
just outside the 90% IBIS error circle, but well within the 99% one. The coordinates of the X-ray
source are RA (J2000) = 03h55m41.79s and
Dec (J2000) = +62d40m57.60s (0.09 arcmin positional uncertainty).
The source 2-10 keV flux is 2.57x10-13 erg cm-2s-1,
assuming a photon index of 1.8.
Consistent with the X-ray position, we find the bright radio source 4C +62.08,
classified in NED as an asymmetric double radio source, with a steep
spectrum of -1.1 (where S&nu&prop&nu&alpha).
It has been observed at various frequencies from 38 MHz with a flux of
1.9 Jy (8C survey) to 4.85 GHz (NRAO 1987 Green Bank radio survey)
with a flux of 191 mJy.
Coincident with the radio and X-ray coordinates, we also find an optical
counterpart in the USNO B-1 catalogue with magnitudes R=18.23, B=19.65 and I=18.07
and an IR counterpart in the 2MASS catalogue, with magnitudes J=16.71, H=16.12 and K=15.28.
Since measurements at 4.85 GHz and in the B magnitude are available, we calculate
the radio loudness of the source (i.e. a source is radio loud if
Kellerman et al. 1989) and find that RL=3.5.
The radio association as well as radio morphology, loudness
and X-ray variability all point to an extragalactic nature for this source.
More in-depth follow-up observations at other wavelengths, in particular in the optical,
are desirable in order to further confirm the nature of this source.