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Title:
An X-Ray Pulsar in the Oxygen-rich Supernova Remnant G292.0+1.8
Authors:
Hughes, John P.; Slane, Patrick O.; Park, Sangwook; Roming, Peter W. A.; Burrows, David N.
Affiliation:
AA(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019 .), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; .), AC(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802.), AD(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802.), AE(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802.)
Publication:
The Astrophysical Journal, Volume 591, Issue 2, pp. L139-L142. (ApJL Homepage)
Publication Date:
07/2003
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: G292.0+1.8, ISM: Individual: Alphanumeric: MSH 11-54, Stars: Pulsars: Individual: Alphanumeric: PSR J1124-5916, Stars: Neutron, ISM: Supernova Remnants, X-Rays: Individual: Alphanumeric: CXOU J112439.1-591620
DOI:
10.1086/377072
Bibliographic Code:
2003ApJ...591L.139H

Abstract

We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period (P=0.13530915 s) is consistent with the extrapolation of the radio pulse period of PSR J1124-5916 for a spin-down rate of P=7.6×10-13 s s-1. The X-ray pulse is single-peaked and broad, with an FWHM width of 0.23P (83°). The pulse-averaged X-ray spectral properties of the pulsar are well described by a featureless power-law model with an absorbing column density NH=3.1×1021 cm-2, a photon index Γ=1.6, and an unabsorbed 0.3-10 keV band luminosity LX=7.2×1032 ergs s-1. We plausibly identify the location of the pulsar's termination shock. Pressure balance between the pulsar wind nebula and the larger synchrotron nebula, as well as lifetime issues for the X-ray-emitting electrons, argue for a particle-dominated pulsar wind nebula that is far from the minimum-energy condition. Upper limits on the surface temperature of the neutron star are at, or slightly below, values expected from ``standard'' cooling curves. There is no optical counterpart to the new pulsar; its optical luminosity is at least a factor of 5 below that of the Crab pulsar.
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