2010/09/07 by D. I. Karasev, D. Karasev, A. Lutovinov +3 · 16 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Bulge #Extinction (optical mineralogy) #Galactic Center #Infrared #Pulsar #Pulsars and Gravitational Waves Research #Spiral galaxy #Stars #Telescope #astro-ph.GA #astro-ph.HE
paper · pdf · doi:10.1111/j.1745-3933.2010.00949.x
published in Monthly Notices of the Royal Astronomical Society Letters 409(1), L69-L73 (Oxford University Press) · 6 pages, 7 figures, will be published in MNRAS
arxiv created 2010/09/07 · openalex publication_date 2010/10/19 · arxiv updated 2015/05/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract Two faint X-ray pulsars, AX J1749.2−2725 and AX J1749.1−2733, located in the direction of the Galactic Centre, were studied in detail using data from the INTEGRAL, XMM–Newton and Chandra observatories in X-rays, the SOFI/NTT instrument in the infrared and the RTT150 telescope in the optical. X-ray positions of both sources were determined with an uncertainty better than ∼1 arcsec, which allowed us to identify their infrared counterparts. From the subsequent analysis of infrared and optical data, we conclude that the counterparts of both pulsars are likely to be massive stars of B0–B3 class located behind the Galactic Centre at distances of 12–20 kpc, depending on the type, probably in the further parts of the Galactic spiral arms. In addition, we investigated the extinction law towards the Galactic bulge and found that it is significantly different from the standard one.