HD 15137 is an intriguing runaway O-type binary system that offers a rare opportunity to explore the mechanism by which it was ejected from the open cluster of its birth. Here, we present recent blue optical spectra of HD 15137 and derive a new orbital solution for the spectroscopic binary and physical parameters of the O star primary. We also present the first XMM-Newton observations of the system. Fits of the EPIC spectra indicate soft, thermal X-ray emission consistent with an isolated O star. Upper limits on the undetected hard X-ray emission place limits on the emission from a proposed compact companion in the system, and we rule out a quiescent neutron star (NS) in the propeller regime or a weakly accreting NS. An unevolved secondary companion is also not detected in our optical spectra of the binary, and it is difficult to conclude that a gravitational interaction could have ejected this runaway binary with a low mass optical star. HD 15137 may contain an elusive NS in the ejector regime or a quiescent black hole with conditions unfavorable for accretion at the time of our observations. © 2010 The American Astronomical Society.
Publication Source (Journal or Book title)
McSwain, M., De Becker, M., Roberts, M., Boyajian, T., Gies, D., Grundstrom, E., Aragona, C., Marsh, A., & Roettenbacher, R. (2010). Multiwavelength observations of the runaway binary HD 15137. Astronomical Journal, 139 (3), 857-864. https://doi.org/10.1088/0004-6256/139/3/857