Observation of the Crab pulsar, PSR 0531 + 21, at 0.2-6.0 MeV with the FIGARO II experiment

Details Observation of the Crab pulsar, PSR 0531 + 21, at 0.2-6.0 MeV with the FIGARO II experiment Observation of the Crab pulsar, PSR 0531 + 21, at 0.2-6.0 MeV with the FIGARO II experiment

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...355..645a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 355, June 1, 1990, p. 645-650. Research supported by CNES and CNR.

Astronomy and Astrophysics

Astronomy

27

Crab Nebula, Gamma Ray Astronomy, Pulsars, Balloon-Borne Instruments, Dark Matter, Light Curve, Pulsar Magnetospheres, Stellar Spectrophotometry, Stellar Structure

Scientific paper

Observations of the Crab pulsar (PSR 0531 + 21) in the energy range 0.2-6 MeV have been made with the balloon-borne Figaro II experiment. The gross appearance of the light curve is characterized by the well-known double-peak structure with a phase separation of 0.4. The data confirm that the second pulse is the dominant feature, and the interpulse region is more luminous than in other energy ranges. Above about 0.5 MeV, an extra structure was detected in the light curve, with two features at a phase lag of 0.4 as the main one. Phase-resolved spectroscopy indicates that the first peak spectrum is concave upward, and the second one is concave downward, while the averaged spectrum is well represented by a single power law with slope 2.2. The good timing accuracy of Figaro made it possible to measure a delay between gamma rays and radio waves of 300 + or - 70 microsec, that if produced by dispersion, implies a value of DM fitting very well the radio measurements 2 months before and after the observation.

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