2001/07/16 by O. C. de Jager, A. Konopelko, de Jager, O. C. +5
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Gamma-ray bursts and supernovae #Nuclear Physics and Applications #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0107278
4 pages, 2 figures, in Proc. 27th ICRC, Hamburg, 07-15 August 2001, OG164
arxiv created 2001/07/16 · openalex publication_date 2001/07/16 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The non-detection of pulsed sub-TeV gamma-rays from EGRET pulsars proves that the EGRET pulsed spectra of all gamma-ray pulsars should terminate at energies below a few hundred GeV. The spectrum of a typical integrated pulse profile predicted by the polar cap model resemble typically a hard component, followed by a super exponential cutoff between 1 MeV (PSR B1509-58) and tens of GeV (e.g. Crab, PSR B1951+32 etc). Using a topological trigger for the H.E.S.S. Telescope System in the non-imaging mode, we show that H.E.S.S. should be able to detect pulsed emission from PSR B1706-44 within a few hours if the cutoff energy is above 30 GeV as suggested by EGRET observations. The recently detected radio pulsar PSR J1837-0604 (pulsar period: 96 ms) associated with the unidentified EGRET source GeV J1837-06010 should also be detectable within a few hours if the source is pulsed and if its cutoff is similar to that of PSR B1706-44. H.E.S.S. should even be able to image middle-aged, low-multiplicity pulsars for which the mean photon energy is expected to be well above 10 GeV. Such observations should provide important constraints on the final evolutionary status of gamma-ray pulsars and millisecond pulsars in general.