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Pulsar optical observation with the Very Large Telescope

Published online by Cambridge University Press:  12 April 2016

A. Ray ,
P. Lundqvist ,
J. Sollerman ,
B. Leibundgut  and
F. Sutaria
A. Ray
Affiliation:
Tata Institute of Fundamental Research, Bombay 400005, India
P. Lundqvist
Affiliation:
Stockholm Observatory, SE-133 36 Saltsjöbaden, Sweden
J. Sollerman
Affiliation:
Stockholm Observatory, SE-133 36 Saltsjöbaden, Sweden
B. Leibundgut
Affiliation:
European Southern Observatory, Garching bei München, Germany
F. Sutaria
Affiliation:
Inter Univ Centre for Astronomy & Astrophysics, Pune 411007, India

Abstract

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Optical data in the V-band gathered with the 8.2m ESO Very Large Telescope (VLT) at the radio interferometric position of PSR 1706-44 are presented. The pulsar is close to a bright star in projection and was not detected. The pulsar magnitude limit must be fainter than V=24.5 for a distance of ≤ from the bright star. In the outer gap model for an aligned rotor the optical flux should scale with the gammaray flux. For pulsars which emit pulsed gamma-rays but are not detected in the optical bands, the synchrotron cutoff frequency for the tertiary photons must be well below the optical frequencies and the magnetic and spin axes may be misaligned.

Type
Part 4. Optical Observations
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 305 - 306
Copyright
Copyright © Astronomical Society of the Pacific 2000

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