High-Energy Gamma-Ray Observations of Two Young, Energetic Radio Pulsars
V. M. Kaspi
J. R. Lackey
J. Mattox
R. N. Manchester
M. Bailes
R. Pace
Abstract
We present results of EGRET observations of the
unidentified high-energy g-ray sources 2EG J1049-5847 (GEV
J1047-5840, 3EG J1048-5840) and 2EG J1103-6106 (3EG J1102-6103). These
sources are spatially coincident with the young, energetic radio
pulsars PSRs B1046-58 and J1105-6107, respectively. We find evidence for an
association between PSR B1046-58 and 2EG J1049-5847. The g-ray pulse
profile, obtained by folding time-tagged photons having energies above
400 MeV using contemporaneous radio ephemerides, has probability of
arising by chance of 1.2 ×10-4 according to the
binning-independent H-test. A spatial analysis of the on-pulse
photons reveals a point source of equivalent significance
10.2s. Off-pulse, the significance drops to 5.8s.
Archival ASCA data show that the only hard X-ray
point source in the 95% confidence error box of the g-ray source is
spatially coincident with the pulsar within the 1¢ uncertainty
(Pivovaroff, Kaspi & Gotthelf 1999). The double peaked g-ray pulse
morphology and leading
radio pulse are similar to those seen for other pulsars
and are well-explained in models in which the g-ray emission is
produced in charge-depleted gaps in the outer magnetosphere. The
inferred pulsed g-ray flux above 400 MeV, (2.5 ±0.6) ×10-10 erg cm-2 s-1, represents 0.011±0.003 of the
pulsar's spin-down luminosity, for a distance of 3 kpc and 1 sr
beaming. For PSR J1105-6107, light curves obtained by folding EGRET
photons using contemporaneous radio ephemerides show no significant
features. We conclude that this pulsar converts less than 0.014 of
its spin-down luminosity into E > 100 MeV g-rays beaming in our
direction (99% confidence), assuming a distance of 7 kpc, 1 sr
beaming and a duty cycle of 0.5.
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On 16 Jul 1999, 09:18.