The X-ray spectrum of the plerionic system PSR B1509-58/MSH 15-52

D. Marsden; P. R. Blanco; D. E. Gruber; W. A. Heindl; M. R. Pelling; L. E. Peterson; R. E. Rothschild; A. H. Rots; K. Jahoda; D. J. Macomb

doi:10.1086/311054

The X-ray spectrum of the plerionic system PSR B1509-58/MSH 15-52

D. Marsden, P. R. Blanco, D. E. Gruber, W. A. Heindl, M. R. Pelling, L. E. Peterson, R. E. Rothschild, A. H. Rots, K. Jahoda, D. J. Macomb

Physics Department

Research output: Contribution to journal › Article › peer-review

27 Scopus citations

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.

Original language	English
Pages (from-to)	L39-L42
Journal	Astrophysical Journal
Volume	491
Issue number	1 PART II
DOIs	https://doi.org/10.1086/311054
State	Published - 1997

Keywords

ISM: individual (MSH 15-52)
Pulsar: individual (PSR B1509-58)
Stars: neutron

Access to Document

10.1086/311054

Cite this

@article{d69c6bc9894c40b8a027e17e2ca8fdce,

title = "The X-ray spectrum of the plerionic system PSR B1509-58/MSH 15-52",

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.",

keywords = "ISM: individual (MSH 15-52), Pulsar: individual (PSR B1509-58), Stars: neutron",

author = "D. Marsden and Blanco, {P. R.} and Gruber, {D. E.} and Heindl, {W. A.} and Pelling, {M. R.} and Peterson, {L. E.} and Rothschild, {R. E.} and Rots, {A. H.} and K. Jahoda and Macomb, {D. J.}",

year = "1997",

doi = "10.1086/311054",

language = "English",

volume = "491",

pages = "L39--L42",

number = "1 PART II",

}

TY - JOUR

T1 - The X-ray spectrum of the plerionic system PSR B1509-58/MSH 15-52

AU - Marsden, D.

AU - Blanco, P. R.

AU - Gruber, D. E.

AU - Heindl, W. A.

AU - Pelling, M. R.

AU - Peterson, L. E.

AU - Rothschild, R. E.

AU - Rots, A. H.

AU - Jahoda, K.

AU - Macomb, D. J.

PY - 1997

Y1 - 1997

N2 - 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.

AB - 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.

KW - ISM: individual (MSH 15-52)

KW - Pulsar: individual (PSR B1509-58)

KW - Stars: neutron

UR - http://www.scopus.com/inward/record.url?scp=21944439738&partnerID=8YFLogxK

U2 - 10.1086/311054

DO - 10.1086/311054

M3 - Article

AN - SCOPUS:21944439738

SN - 0004-637X

VL - 491

SP - L39-L42

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART II

ER -

The X-ray spectrum of the plerionic system PSR B1509-58/MSH 15-52

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this