Optical Spectroscopy of Gamma-ray Binaries

Details Optical Spectroscopy of Gamma-ray Binaries Optical Spectroscopy of Gamma-ray Binaries

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21341008a&link_type=abstract

American Astronomical Society, AAS Meeting #213, #410.08; Bulletin of the American Astronomical Society, Vol. 41, p.212

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Scientific paper

There are currently only five known high mass x-ray binaries with very high energy MeV-TeV emission, or "gamma-ray binaries". These systems consist of O-type or B-type stars and a neutron star or black hole companion. There are two models for the origin of the gamma-ray emission. One suggests that the companion is an accreting neutron star or black hole. The other predicts a pulsar for the companion star, with relativistic winds that collide with the stellar winds. We are currently involved in a multiwavelength campaign to study the stellar/companion interactions and determine the mechanism producing the high energy emission in gamma-ray binaries. We present optical spectra of LS5039 from the CTIO 1.5m telescope and discuss the orbital parameters and stellar wind strengths. We also present new KPNO Coudé Feed spectra of LS I +61 303 and HD 259440, the proposed optical counterpart of the new gamma-ray binary HESS J0632+057, for the first detailed optical investigation of that system.
We gratefully acknowledge support from NASA grant # NNX08AV70G and Lehigh University.

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