Titlebook: Very High Energy Gamma Ray Astronomy; K. E. Turver Book 1987 D. Reidel Publishing Company, Dordrecht, Holland 1987 astronomy.astrophysics.

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antenna

TeV Observations of Her X-l at the Whipple Observatory: 1984–1985en distinct episodes of emission were seen, ranging in duration from 25 to 80 minutes, totalling 7% of all observations. Evidence is presented which suggests that the gamma-ray source is not always coincident with the X-ray source; in particular, the strongest effect was observed after the pulsar en

Indelible

VHE Gamma Rays from the X-Ray Pulsar 4U0115+63Three intervals of ≤1000 seconds exhibited significant (chance probability ≤ 10.) pulsation at the characteristic 3.6 second period of the neutron star member of the binary system. The average peak flux above 0.2 TeV for these observations was (2.0 ± 0.4) x 10. cm. sec.. These observations are consi

etiquette

Pulsed TeV Gamma Rays from 4u0115+635 and January 1986. These observations were grouped into nine intervals of three days or less. One interval shows significant pulsation at the 3.6 second spin period of the neutron star member of the binary system at a flux level of (1.5±0.4)xl0. photons above 0.6 TeV cm.s.. Thus these observations