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 language||English (US)|
|Journal||Astronomy and Astrophysics|
|State||Published - Jul 1 1998|
- Pulsars: individual (Geminga) techniques: 2-d photon-counting detectors
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science