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Mass and Orbit Constraints of the Gamma-ray Binary LS 5039

Published online by Cambridge University Press:  23 April 2012

T. Szalai ,
G. E. Sarty ,
L. L. Kiss ,
J. M. Matthews ,
J. Vinkó  and
C. Kiss
T. Szalai
Affiliation:
Department of Optics and Quantum Electronics, University of Szeged, Dóm tér 9., Szeged H-6720, Hungary; email: szaszi@titan.physx.u-szeged.hu
G. E. Sarty
Affiliation:
Royal Astronomical Society of Canada, Saskatoon Centre, P.O. Box 317, RPO University, Saskatoon, SK S7N 4J8, Canada Department of Physics and Engineering Physics, University of Saskatchewan, Saskatoon, SK S7N 5E2, Canada
L. L. Kiss
Affiliation:
Konkoly Observatory of the Hungarian Academy of Sciences, H-1525 Budapest, P.O. Box 67, Hungary
J. M. Matthews
Affiliation:
Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada
J. Vinkó
Affiliation:
Department of Optics and Quantum Electronics, University of Szeged, Dóm tér 9., Szeged H-6720, Hungary; email: szaszi@titan.physx.u-szeged.hu
C. Kiss
Affiliation:
Konkoly Observatory of the Hungarian Academy of Sciences, H-1525 Budapest, P.O. Box 67, Hungary
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Abstract

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We present the results of space-based photometric and ground-based spectroscopic observing campaigns on the γ-ray binary LS 5039. The new orbital and physical parameters of the system are similar to former results, except we found a lower eccentricity. Our MOST-data show that any broad-band optical photometric variability at the orbital period is below the 2 mmag level. Light curve simulations support the lower value of eccentricity and imply that the mass of the compact object is higher than 1.8 M⊙.

Keywords

binaries: spectroscopicstars: individual (LS 5039)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 331 - 332
Copyright
Copyright © International Astronomical Union 2012

References

Aragona, C., McSwain, M. V., Grundstrom, E. D., et al. , 2009, ApJ, 698, 514CrossRefGoogle Scholar
Casares, J., Ribó, M., Ribas, I., et al. , 2005, MNRAS, 364, 899CrossRefGoogle Scholar
Casares, J., Corral-Santana, J. M., Herrero, A., et al. , 2010, arXiv:1012.4351Google Scholar
Kaufer, A., Stahl, O., Tubbesing, S., et al. , 1999, The Messenger, 95, 8Google Scholar
Paredes, J. M., Martí, J., & Ribó, M., Massi, M., 2000, Science, 288, 2340CrossRefGoogle Scholar
Sarty, G. E., Szalai, T., Kiss, L. L., et al. , 2011, MNRAS, 411, 1293 (S11)CrossRefGoogle Scholar
Wilson, R. E. & van Hamme, W. 2003, Computing Binary Stars Observables, Ver. 4.Google Scholar