Open AccessA search for the binary companion to PSR J1740–3052
Author(s) -
Tam C. R.,
Stairs I. H.,
Wagner S.,
Kramer M.,
Manchester R. N.,
Lyne A. G.,
Camilo F.,
D'Amico N.
Publication year - 2010
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2010.16785.x
Subject(s) - physics , astrophysics , astronomy , pulsar , telescope , radial velocity , proper motion , binary pulsar , star (game theory) , binary star , millisecond pulsar , stars
We present results of near‐infrared spectroscopy of the late‐type star coincident with the young pulsar PSR J 1740− 3052. High‐spectral‐resolution K ‐band ( ∼2.2 μ m) 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 J 1740− 3052 is most likely a massive B‐type star that has been obscured by the bright late‐type star in the foreground.