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 (similar to 2.2 mu 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(circle dot). We therefore conclude that the observed star is likely to be a foreground object. No sign of the previously reported Brackett-gamma 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.
A search for the binary companion to PSR J1740-3052
D'AMICO, NICOLO'
2010-01-01
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 (similar to 2.2 mu 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(circle dot). We therefore conclude that the observed star is likely to be a foreground object. No sign of the previously reported Brackett-gamma 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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