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 Porb (=15.7 d) versus Ppulse "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. © ESO 2007.
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In’t Zand, J. J. M., Kuiper, L., Den Hartog, P. R., Hermsen, W., & Corbet, R. H. D. (2007). A probable accretion-powered X-ray pulsar in IGR J00370+6122. Astronomy and Astrophysics, 469(3), 1063–1068. https://doi.org/10.1051/0004-6361:20077189