A search for the binary companion to PSR J1740–3052

Authors

  • C. R. Tam,

    Corresponding author
    1. Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver BC V6T 1Z1, Canada
      E-mail: ctam@phas.ubc.ca
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  • I. H. Stairs,

    1. Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver BC V6T 1Z1, Canada
    2. Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia
    3. Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Mail 39, PO Box 218, Hawthorn, Vic 3122, Australia
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  • S. Wagner,

    1. Landessternwarte Königstuhl, Königstuhl 12, 69117 Heidelberg, Germany
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  • M. Kramer,

    1. Jodrell Bank Observatory, University of Manchester, Macclesfield, Cheshire SK11 9DL
    2. MPI für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
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  • R. N. Manchester,

    1. Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia
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  • A. G. Lyne,

    1. Jodrell Bank Observatory, University of Manchester, Macclesfield, Cheshire SK11 9DL
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  • F. Camilo,

    1. Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA
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  • N. D'Amico

    1. INAF-Osservatorio Astronomico di Cagliari, loc. Poggio dei Pini, strada 54, I-09012 Capoterra, Italy
    2. Dipartimento di Fisica, Università di Cagliari, Cittadella Universitaria, I-09042 Monserrato, Italy
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E-mail: ctam@phas.ubc.ca

ABSTRACT

We present results of near-infrared spectroscopy of the late-type star coincident with the young pulsar PSR J1740−3052. High-spectral-resolution K-band (∼2.2 μm) observations were obtained in 2003 with the Infrared Spectrometer and Array Camera instrument on the Very Large Telescope and with Phoenix on the Gemini Telescope. We find no consistent evidence of a radial velocity shift in the star compatible with the known pulsar orbit, setting a limit on the minimum mass of the star, if it is the companion, of 60  M. We therefore conclude that the observed star is likely to be a foreground object. No sign of the previously reported Brackett-γ emission was found in this analysis. Our findings support previous suggestions that the companion to PSR J1740−3052 is most likely a massive B-type star that has been obscured by the bright late-type star in the foreground.

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