Prospects of observing pulsed radiation from gamma-ray pulsars with H.E.S.S

Details Prospects of observing pulsed radiation from gamma-ray pulsars with H.E.S.S Prospects of observing pulsed radiation from gamma-ray pulsars with H.E.S.S

2000-10-10

arxiv.org/abs/astro-ph/0010179v1

AIP Conf.Proc. 558 (2001) 613-616

Astronomy and Astrophysics

Astrophysics

4 pages, 2 figures, Proceedings of the Heidelberg International Symposium on High Energy Gamma-Ray Astronomy

Scientific paper

10.1063/1.1370835

Observations and theoretical studies have demonstrated that the pulsed spectra of all gamma-ray pulsars terminate at energies below a few hundred GeV. In most cases we expect this cutoff energy E_o to be around 10 GeV. Only with next generation ground-based gamma-ray telescopes, which are expected to have non-zero trigger probabilities near 10 GeV, can we expect to detect pulsations. The large gamma-ray fluxes below E_o, together with the associated sharp pulse profiles, compensate for the lack of imaging capability near threshold. For H.E.S.S. we find that the pulsed component of PSR B1706-44 should be detectable near threshold, whereas the unidentified GeV EGRET sources should be detectable if the superexponential cutoff energy is larger that approximately 30 GeV for relatively hard pulsar photon spectra (~E^-1.5).

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