Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· On-line Data
· References in the article
· Citations to the Article (35) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (3)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
The pulsed hard X-ray spectrum of PSR B1509-58
Authors:
Matz, S.; Ulmer, M. P.; Grabelsky, D. A.; Purcell, W. R.; Grove, J. E.; Johnson, W. N.; Kinzer, R. L.; Kurfess, J. D.; Strickman, M. S.; Jung, G. V.
Affiliation:
AA(Northwestern Univ., Evanston, IL, US), AB(Northwestern Univ., Evanston, IL, US), AC(Northwestern Univ., Evanston, IL, US), AD(Northwestern Univ., Evanston, IL, US), AE(Naval Research Lab., Washington, DC, US), AF(Naval Research Lab., Washington, DC, US), AG(Naval Research Lab., Washington, DC, US), AH(Naval Research Lab., Washington, DC, US), AI(Naval Research Lab., Washington, DC, US), AJ(Naval Research Lab., Washington, DC, US)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 1, p. 288-291 (ApJ Homepage)
Publication Date:
10/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
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
DOI:
10.1086/174727
Bibliographic Code:
1994ApJ...434..288M

Abstract

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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints