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Pulsar optical observation with the Very Large Telescope

  • A. Ray (a1), P. Lundqvist (a2), J. Sollerman (a2), B. Leibundgut (a3) and F. Sutaria (a4)...

Abstract

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.

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Copyright

References

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Chakrabarty, D., Kaspi, V.M. 1998, ApJ, 498, L37 (CK98)
Cheng, K.S., Ho, C., Ruderman, M.A. 1986, ApJ, 300, 500
Lundqvist, P., Sollerman, J., Ray, A., Leibundgut, B. & Sutaria, F., 1999, A & A, 343, L15
Ray, A., Harding, A.K., Strickman, M.S. 1999, ApJ, 513, 919
Thompson, D.J. et al. 1996, ApJ, 385, 465
Thompson, D.J. et al. 1999, ApJ, in press (astro-ph/9811219)
Usov, V.V. 1994, ApJ 427, 394

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