The Astrophysical Journal · 1988 · 15 citations · 0 references
Natural SciencesAstronomyPhysicsAstrophysicsGamma-ray AstronomyObservational AstronomyGamma-ray SourcesGamma-ray TelescopesGround-based Gamma-ray ObservatoriesHigh-energy Astrophysical SourcesPulsar AstronomyCore-collapse SupernovaeGamma-ray Emission MechanismsGamma-ray PulsarsHigh-energy Gamma-ray AstronomyPulsar ObservationsVery-high-energy Gamma-ray Astronomy
If a pulsar remains in the center of the expanding shell of SN 1987A, then it is possible that it will be seen first in very high energy (VHE) gamma rays, once the debris has cleared. A search for 400 GeV gamma rays from SN 1987A has been conducted using the Narrabri gamma-ray telescope, starting with a fortuitous observation within 5 hr of the core collapse in 1987 February, through to a more extensive program of observations up to 1988 April. The pulsar, if present, has not been detected yet as a VHE gamma-ray source, and this places some limits to the possible pulsar parameters. A luminosity limit of 4 x 10^38^ ergs s^-1^ (significant at the 3σ level) was obtained for the emission of gamma rays of energy greater than 400 GeV immediately following the collapse. Subsequent observations throughout 1987 indicate continued validity of this limit. In 1988 January-February, as the possibility of the penetration of VHE gamma rays increased, a limit of 7 x 10^37^ ergs s^-1^ has been placed on the luminosity. This is beginning to constrain certain models for high-energy proton production in pulsars, suggested on phenomenological grounds.