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Optical spectroscopy of X-ray source IGR J22534+6243

ATel #4248; N. Masetti (INAF/IASF Bologna), E. Jimenez-Bailon (UNAM, Mexico City), V. Chavushyan (INAOE, Puebla), P. Parisi, A. Bazzano (INAF/IAPS, Rome), R. Landi (INAF/IASF, Bologna), and A. J. Bird (Univ. Southampton)
on 10 Jul 2012; 15:18 UT
Credential Certification: Nicola Masetti (masetti@iasfbo.inaf.it)

Subjects: Optical, X-ray, Binary, Neutron Star, Star, Pulsar

Following the discovery of a 46.6 X-ray periodicity (ATel #4240, #4241) from the X-ray source IGR J22534+6243 (Krivonos et al. 2012, arXiv:1205.3941; ATel #4166), we analyzed spectroscopic data of its putative optical counterpart (ATel #4166) which were obtained using the 2.1m telescope of the Observatorio Astronomico Nacional (San Pedro Martir, Baja California, Mexico) equipped with a Boller & Chivens spectrograph.

Observations were acquired starting at 10:52 UT of 22 June 2012, for a total exposure time of 1800 s.

The 4000-8000 Angstroms optical spectrum shows a highly reddened (but otherwise intrinsically blue) continuum with superimposed Halpha, Hbeta and He I emissions at redshift zero, together with several absorption lines of Galactic interstellar origin. We measure the equivalent widths of Halpha and Hbeta as 31.8 +- 1.6 and 3.4 +- 0.5 Angstroms, respectively.

The optical spectral appearance of the counterpart is thus typical of an absorbed Galactic high mass X-ray binary (HMXB), which confirms the HMXB nature for IGR J22534+6243 as suggested in ATel #4240.