The pulsed hard X-ray spectrum of PSR B1509-58

Details The pulsed hard X-ray spectrum of PSR B1509-58 The pulsed hard X-ray spectrum of PSR B1509-58

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...434..288m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 1, p. 288-291

Computer Science

Numerical Analysis

38

Binary Stars, Gamma Rays, Pulsars, Pulse Amplitude, Supernova Remnants, X Ray Spectra, X Ray Stars, Collimators, Gamma Ray Observatory, Numerical Analysis, Satellite-Borne Instruments, Scaling

Scientific paper

Oriented Scintillation Spectrometer Experiment (OSSE) observed the 150 ms X-ray pulsar PSR B1509-58 m the supernova remnant MSH 15-52 for 4 weeks in 1992. The pulsed spectrum from 50 keV to 5 MeV is well represented by a single-power-law photon spectrum of the form (3.14 +/- 0.16) x 10-6 x (E/118.5 keV)-1.68 +/- -0.09 photons cm-2s-1keV-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 2 times higher than we observe in the approximately 55-170 keV energy band. This requires a break to a steeper spectrum somewhere in the intermediate energy range (approximately 20-80 keV). The spectrum must soften again at higher energies or the pulsar would have easily been detected by EGRET, COS B, and SAS 2.

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