Identification of an X-Ray Pulsar in the BeXRB System IGR J18219-1347

B. O'Connor, E. Göǧüş, D. Huppenkothen, C. Kouveliotou, N. Gorgone, L. J. Townsend, A. Calamida, A. Fruchter, D. A.H. Buckley, M. G. Baring, J. A. Kennea, G. Younes, Z. Arzoumanian, E. Bellm, S. B. Cenko, K. Gendreau, J. Granot, C. Hailey, F. Harrison, D. HartmannL. Kaper, A. Kutyrev, P. O. Slane, D. Stern, E. Troja, A. J. Van Der Horst, R. A.M.J. Wijers, P. Woudt

نتاج البحث: نشر في مجلةمقالةمراجعة النظراء


We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219-1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with P spin = 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10-15 kpc for the source. The broadband X-ray spectrum (1.5-50 keV) of the source is described by an absorbed power law with a photon index Γ ∼0.5 and a cutoff energy at ∼13 keV.

اللغة الأصليةالإنجليزيّة
رقم المقال139
دوريةAstrophysical Journal
مستوى الصوت927
رقم الإصدار2
المعرِّفات الرقمية للأشياء
حالة النشرنُشِر - 1 مارس 2022

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© 2022. The Author(s). Published by the American Astronomical Society.


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