EGRET observations of the VELA pulsar, PSR0833-45

Details EGRET observations of the VELA pulsar, PSR0833-45 EGRET observations of the VELA pulsar, PSR0833-45

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...289..855k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 289, no. 3, p. 855-867

Astronomy and Astrophysics

Astronomy

105

Energy Spectra, Gamma Ray Spectra, Pulsars, Radio Observation, Stellar Luminosity, Data Correlation, Gamma Ray Observatory, Light Curve, Sky Surveys (Astronomy), Spectrum Analysis

Scientific paper

During the all sky survey (May 1991 to November 1992) of the Compton Gamma Ray Observatory, the Vela pulsar PSR0833-45 was in the field of view of the Energetic Gamma Ray Experiment Telescope (EGRET) in ten separate viewing periods. The pulsar was detected in each one. The average intensity from 100 MeV to 2GeV was (7.8 +/- 1.0) x 10-6 photons /sq cm/s, which indicates that the pulsar in the years 1991/92 was in a state comparable to the low fluxes observed in 1977-1980. No significant changes in intensity were detected during the EGRET observations. The total spectrum of PSR0833-45 measured by EGRET can be described by a power-law with index -1.70 +/- 0.02 over the range 30 MeV to 2 GeV. The extrapolation of this spectrum into the 3-30 MeV range agrees with the observations by COMPTEL. Above 2-4 GeV EGRET detects a strong spectral break. The lightcurves obtained show a familiar structure in the phase histogram: two peaks separated by 0.424 +/- 0.002 in phase with considerable emission in the phase interval between the peaks. The first gamma ray peak maximum trails the single radio peak maximum by 10.54 +/- 0.09 ms (= 0.118 +/- 0.001 in phase). The widths of the emission peaks (FWHM) are 2.7 ms for the first peak (0.03 phase) and 4.1 ms for the second peak (0.05 phase). The widths are approximately constant below a GeV, but show a tendency to become narrower at higher energies. The statistics available for the Vela observations allow for a division of the lightcurve into eight phase intervals. The emission peak cores (central FWHM) with leading and trailing wings and two interval regions were defined and spectra were derived for all parts of the lightcurve. The energy spectra for the eight phase intervals show significant differences: the first peak (approximately E-1.81 +/- 0.04) is somewhat softer than the second peak (approximately E-1.71 +/- 0.03); the wings attached to each peak show softer spectra than the core of the peaks; the interval emission has the hardest spectrum (approximately E-1.52 +/- 0.03).

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