The Spectrum of the Large Magellanic Cloud Pulsar B0540-69

Details The Spectrum of the Large Magellanic Cloud Pulsar B0540-69 The Spectrum of the Large Magellanic Cloud Pulsar B0540-69

Sep 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...486l..99h&link_type=abstract

Astrophysical Journal Letters v.486, p.L99

Astronomy and Astrophysics

Astronomy

24

Stars: Pulsars: Individual Alphanumeric: B0540-69, Ultraviolet: Stars

Scientific paper

A prism spectrum of PSR B0540-69, the 50 ms pulsar in the Large Magellanic Cloud, was obtained with the Faint Object Spectrograph on the Hubble Space Telescope. This is only the second pulsar spectrum that has been observed in the optical. The 2500--5500 A spectrum shows a smooth continuum with several broad emission lines. The lines are emitted by the extended nebula surrounding B0540-69. Less than 30% of the total flux in the spectrum can be contributed by the synchrotron nebula surrounding the pulsar; the time-averaged emission from the pulsar must be the dominant source of the continuum. The observed spectral index, alpha , of the continuum, where flux density S nu = K nu alpha mu Jy, is -2.5 +/- 0.2 between 2500 and 4500 A . Using E(B - V) = 0.20 +/- 0.05 gives a de-extincted spectral index alpha 0 = -1.6 +/- 0.4. This intrinsic spectral index is significantly different from that of the Crab pulsar in the optical alpha 0 = 0.11 +/- 0.13. Unless E(B - V) ~ 0.5, the intrinsic spectral index of time-averaged pulsar radiation must vary as much from pulsar to pulsar in the high-frequency regime as it does in the radio.

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