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Title:
The X-Ray Spectrum of the Plerionic System PSR B1509$-$58/MSH 15$-$52
Authors:
Marsden, D.; Blanco, P. R.; Gruber, D. E.; Heindl, W. A.; Pelling, M. R.; Peterson, L. E.; Rothschild, R. E.; Rots, A. H.; Jahoda, K.; Macomb, D. J.
Publication:
Astrophysical Journal Letters v.491, p.L39 (ApJL Homepage)
Publication Date:
12/1997
Origin:
APJ
ApJ Keywords:
ISM: INDIVIDUAL ALPHANUMERIC: MSH 15$-$52, STARS: PULSARS: INDIVIDUAL ALPHANUMERIC: PSR 1509$-, 58, STARS: NEUTRON
DOI:
10.1086/311054
Bibliographic Code:
1997ApJ...491L..39M

Abstract

We present the results of observations of the PSR B1509-58/MSH 15-52 system in X-rays (2-250 keV) by the Rossi X-Ray Timing Explorer. The spectra of the peak of the pulsed component (radio phase 0.17-0.53) is fitted by a power law of photon index 1.36+/-0.01 , with no evidence of a high-energy spectral break seen up to ~200 keV. For the off-pulse spectral component, the spectrum from 2-250 keV is fitted by a power law of photon index 2.215+/-0.005 . An iron emission line at 6.7 keV with an equivalent width of 129 eV improves the fit, but only at a marginal significance. Thermal bremsstrahlung and Raymond-Smith models produce much worse fits to the unpulsed data. The lack of a high-energy spectral break in the pulsed emission implies an efficiency of >=3% in the conversion of pulsar spin-down energy to pulsed X-rays in the system.
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