期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 479, 期 4, 页码 4849-4860出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1775
关键词
astrometry; parallaxes; proper motions; pulsars: individual: PSR B1259; 63; radio continuum: stars; gamma-rays: stars
资金
- Australian Government
- National Collaborative Research Infrastructure Strategy
- Government of Western Australia
- Science and Industry Endowment Fund
- Pawsey Supercomputing Centre
- Gaia Multilateral Agreement
- Australian Research Council Future Fellowships [FT140101082, FT150100415]
- Spanish Ministerio de Economia, Industria y Competitividad (MINEICO/FEDER, UE) [FPA2015-69210-C6-2-R, AYA2016-76012-C3-1-P, MDM-2014-0369]
- Catalan DEC grant [2017 SGR 643]
- NSF Physics Frontiers Center [1430284]
The pulsar/massive star binary system PSR B1259-63/LS 2883 is one of the best-studied gamma-ray binaries, a class of systems whose bright gamma-ray flaring can provide important insights into high-energy physics. Using the Australian Long Baseline Array, we have conducted very long baseline interferometric observations of PSR B1259-63 over 4.4 years, fully sampling the 3.4-year orbital period. From our measured parallax of 0.38 +/- 0.05 mas-we use a Bayesian approach to infer a distance of 2.6(-0.3)(+0.4) kpc. We find that the binary orbit is viewed at an angle of 154 +/- 3 degrees to the line of sight, implying that the pulsar moves clockwise around its orbit as viewed on the sky. Taking our findings together with previous results from pulsar timing observations, all seven orbital elements for the system are now fully determined. We use our measurement of the inclination angle to constrain the mass of the stellar companion to lie in the range 15-31 M-circle dot. Our measured distance and proper motion are consistent with the system having originated in the Cen OB1 association and receiving a modest natal kick, causing it to have moved similar to 8 pc from its birthplace over the past similar to 3 x 10(5) years. The orientation of the orbit on the plane of the sky matches the direction of motion of the X-ray synchrotron-emitting knot observed by the Chandra X-ray Observatory to be moving away from the system.
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