Possible pulsed optical emission from Geminga

A. Shearer, A. Golden, S. Harfst, R. Butler, R. M. Redfern, C. M.M. O'Sullivan, G. M. Beskin, S. I. Neizvestny, V. V. Neustroev, V. L. Plokhotnichenko, M. Cullum, A. Danks

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Abstract

We present optical data which suggests that G″, the optical counterpart of the γ-ray pulsar Geminga, possibly pulses in B with a period of 0.237 seconds. The similarity between the optical pulse shape and the γ-ray light curve indicates that a large fraction of the optical emission is non-thermal in origin - contrary to recent suggestions based upon the total optical flux. The derived magnitude of the pulsed emission is mB = 26.0 ± 0.4. Whilst it is not possible to give an accurate figure for the pulsed fraction (due to variations in the sky background) we can give an 1 σ upper limit of mB ≈ 27 for the unpulsed fraction.

Original languageEnglish (US)
Pages (from-to)L21-L24
JournalAstronomy and Astrophysics
Volume335
Issue number1
Publication statusPublished - Jul 1 1998

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Keywords

  • Pulsars: individual (Geminga) techniques: 2-d photon-counting detectors

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Shearer, A., Golden, A., Harfst, S., Butler, R., Redfern, R. M., O'Sullivan, C. M. M., ... Danks, A. (1998). Possible pulsed optical emission from Geminga. Astronomy and Astrophysics, 335(1), L21-L24.