The Pulsed Hard X-Ray Spectrum of PSR B1509-58
NAVAL RESEARCH LAB WASHINGTON DC E O HULBURT CENTER FOR SPACE RESEARCH
Pagination or Media Count:
OSSE observed the 150 ms X-ray pulsar PSR B1509-58 in the supernova remnant MSH 15-52 for four weeks in 1992. The pulsed spectrum from 50 keV to 5 MeV is well-fit by a single power law photon spectrum of the form 3.14 plus or minus 0.16 x 10exp 6 xE118.5 keVexp-1.68 plus or minus 0.09 photons cmexp-2 sexp-1 keVexp -1. this is significantly harder than the Crab pulsar spectrum in this energy range. The Ginga soft X-ray spectrum 2-60 keV reported by Kawai et al. Is significantly harder than the observed OSSE spectrum and predicts a flux two times higher than we observe in the 55 -170 keV energy band. This requires a break to a steeper spectrum somewhere in the intermediate energy range 40 - 80 keV. The spectrum must soften again at higher energies or the pulsar would have easily been detected by EGRET, COS B, and SAS-2.
- Nuclear Physics and Elementary Particle Physics