Volume 508, Number 2, December III 2009
|Page(s)||889 - 894|
|Section||Stellar structure and evolution|
|Published online||15 October 2009|
The nature of the X-ray binary IGR J19294+1816 from INTEGRAL, RXTE, and Swift observations
Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot (UMR 7158), CEA Saclay, DSM/IRFU/SAp, 91191 Gif-sur-Yvette, France e-mail: firstname.lastname@example.org
2 Space Science Laboratory, 7 Gauss Way, University of California, Berkeley, C1 94720-7450, USA
3 INAF-IASF, Sezione di Milano, via Bassini 15, 20133 Milano, Italy
Accepted: 9 October 2009
We report the results of a high-energy multi-instrumental campaign with INTEGRAL, RXTE, and Swift of the recently discovered INTEGRAL source IGR J19294+1816. The Swift/XRT data allow us to refine the position of the source to = = +18° 18′38.4″ (±3.5″), which in turn permits us to identify a candidate infrared counterpart. The Swift and RXTE spectra are well fitted with absorbed power laws with hard (Γ ~ 1) photon indices. During the longest Swift observation, we obtained evidence of absorption in true excess to the Galactic value, which may indicate some intrinsic absorption in this source. We detected a strong (%) pulsation at 12.43781 (±0.00003) s that we interpret as the spin period of a pulsar. All these results, coupled with the possible 117 day orbital period, point to IGR J19294+1816 being an HMXB with a Be companion star. However, while the long-term INTEGRAL/IBIS/ISGRI 18-40 keV light curve shows that the source spends most of its time in an undetectable state, we detect occurrences of short (~ s) and intense flares that are more typical of supergiant fast X-ray transients. We therefore cannot make firm conclusions on the type of system, and we discuss the possible implications of IGR J19294+1816 being an SFXT.
Key words: X-rays: binaries / accretion, accretion disks / stars: individual: IGR J19294+1816 / stars: individual: IGR J11215-5952 / stars: individual: IGR J18483-0311
© ESO, 2009
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