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XMM-Newton refinement of the positions of two INTEGRAL sources

ATel #3125; J. Rodriguez (CEA Saclay, AIM-SAp, France), A. Bodaghee & J. A. Tomsick (SSL UC Berkeley, USA)
on 27 Jan 2011; 17:24 UT
Credential Certification: Jerome Rodriguez (jrodriguez@cea.fr)

Subjects: Infra-Red, Optical, X-ray, AGN, Binary, Quasar, Star, Transient, Variables, Pulsar

We report the identification and positional refinement of two INTEGRAL sources with the XMM-Newton satellite. For both sources we analyzed the MOS 1 and MOS 2 images and obtained the best X-ray position with the standard tools provided by the XMM Standard Analysis Software.

IGR J18027-1455:
A precise analysis of the XMM data of this Sey 1 AGN is presented in Panessa et al. 2008, A&A, 483, 151. The authors, however, did not report the refined position obtained with XMM-Newton. Only one bright counterpart is found within the IBIS error box of this source. The averaged MOS 1/2 position is :
RA = 18h 02m 47.32s
Dec = -14deg 54' 54.6"
The error is dominated by a systematic uncertainty of 3.4" at the 90% confidence level. This position is compatible with all previously suggested counterparts, including 1RXS J180245.5-145432 (Combi et al. 2004 ATel #246), although at the ~2 sigma level in the latter case.

IGR J19284+0107:
Very little is known about this source that was first mentioned in the 2nd IBIS catalogue. A single X-ray source is found just on the outer edge of the IBIS 90% error box at an averaged MOS 1/2 position of: RA=19h 28 29.6s
Dec=+01deg 06' 42.4"
with a total uncertainty of 3.8" at 90%. We did not find counterparts in the Rosat, 2MASS, 2MAS X, NVSS, USNO-B1.0, and NED catalogues within the XMM-Newton error box. We, however, remark the presence of 2MASS J19282921+0106418 (J=15.9, H=15.7, Ks=15.3) and USNO-B1.0 0911-0445937 (B=18.2, R=16.4, I=16.7) at respectively 5.8" (at ~2.6 sigma) and 5.4" (2.4 sigma) from the X-ray position. The X-ray source is too faint for a meaningful spectral analysis to be performed. A chance association of the X-ray and IGR sources cannot be completely excluded.

Observations at other wavelengths are encouraged to unveil the nature of the second object.

This research has made use of the IGR Sources page maintained by J. Rodriguez & A. Bodaghee (http://irfu.cea.fr/Sap/IGR-Sources/).