Discovery and interpretation of an X-ray period in the galactic center source CXOGC J174536.1-285638

Creators: Mikles, Valerie J.; Eikenberry, Stephen S.; Muno, Michael P.; Bandyopadhyay, Reba M.

Others:: Bandyopadhyay, Reba M.; Wachter, Stefanie; Gelino, Dawn; Gelino, Christopher R.

Abstract

We present X-ray and infrared observations of the X-ray source CXOGC J174536.1-285638 (hereafter, Edd-1). The spectrum of the X-ray source has a very prominent Fe 6.7 keV emission feature and the infrared counterpart has strong Brackett series and HeI emission. The presence of CIII, NIII, and HeII in the infrared spectrum indicates a binary system. Analysis of the combined Chandra and XMM light curves suggests a possible period of 189±6 days; if we interpret this as an orbital period, we can place constraints on the nature of the primary star and the mass ratio of the system. We compare the source to several massive star systems including both known colliding wind binaries and high-mass X-ray binaries. The X-ray and infrared luminosities are consistent with these types of systems, however, Edd-1 cannot be definitively classified by color alone.

Additional Information

© 2008 American Institute of Physics. The authors make use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Authors are Visiting Astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the National Space Science, Planetary Astronomy Program. Many thanks to the IRTF support staff who assisted us with remote observing on this run. VJM, SSE, and RMB are supported in part by an NSF Grant (AST-0507547). MPM was supported by the National Aeronautics and Space Administration through Chandra Award Number GO6-7135 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060.

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