A probable accretion-powered X-ray pulsar in IGR J00370+6122

Details A probable accretion-powered X-ray pulsar in IGR J00370+6122 A probable accretion-powered X-ray pulsar in IGR J00370+6122

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...469.1063i&link_type=abstract

Astronomy and Astrophysics, Volume 469, Issue 3, July III 2007, pp.1063-1068

Astronomy and Astrophysics

Astrophysics

4

X-Rays: Binaries, X-Rays: Individuals: Igr J00370+6122, X-Rays: Individuals: 1Rxs J003709.6+612131, X-Rays: Individuals 1Rxs J003357.9+612645, Accretion, Accretion Disks, Stars: Neutron

Scientific paper

Serendipitous and dedicated observations with the Rossi X-ray Timing Explorer (RXTE) and the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) were analyzed to study the transient high-mass X-ray binary IGR J00370+6122, in particular to search for an accretion-powered pulsar as companion to the optically identified (Reig et al. 2005, A&A, 440, 637) B0.5 II-III donor star. Highly variable fluxes were measured in the RXTE data during outbursts of up to 2.2 × 10-10 erg cm-2 s-1 (3-20 keV; averaged over 1 h). During a 1-h time span with RXTE flaring activity was detected with an oscillating signal repeating 7 times. Epoch folding reveals a 346 ± 6 s period. We propose that this is the period of the putative pulsar. This measurement puts the source in the wind-fed accretion region of the P_orb (=15.7 d) versus P_pulse “Corbet” diagram. The 3 to 60 keV flare spectrum was modeled with an absorbed power law and the absorption column was found to be 15-20 times larger than the interstellar value and the value obtained for the optical counterpart, suggesting an accretor embedded in the wind of the donor star.

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