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Title:
A Pulsar Wind Nebula in the Oxygen-rich Supernova Remnant G292.0+1.8
Authors:
Hughes, John P.; Slane, Patrick O.; Burrows, David N.; Garmire, Gordon; Nousek, John A.; Olbert, C. M.; Keohane, J. W.
Affiliation:
AA(; Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8109 .), 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.), AF(; North Carolina School of Science and Mathematics, 1219 Broad Street, Durham, NC 27705.), AG(; North Carolina School of Science and Mathematics, 1219 Broad Street, Durham, NC 27705.)
Publication:
The Astrophysical Journal, Volume 559, Issue 2, pp. L153-L156. (ApJL Homepage)
Publication Date:
10/2001
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: SNR G292.0+1.8, ISM: Individual: Alphanumeric: MSH 11-54, Stars: Pulsars: General, Shock Waves, ISM: Supernova Remnants, X-Rays: ISM
DOI:
10.1086/323974
Bibliographic Code:
2001ApJ...559L.153H

Abstract

Using the Chandra X-Ray Observatory, we have discovered a diffuse, center-filled region of hard X-ray emission within the young, oxygen-rich supernova remnant (SNR) G292.0+1.8. Near the peak of this diffuse emission lies a pointlike source of X-ray emission that is well described by an absorbed power-law spectrum with photon index 1.72+/-0.09. This source appears to be marginally extended; its extent of 1.3" (FWHM) is greater than that of a nearby serendipitous X-ray source with FWHM=1.1". This is strong evidence for the presence within SNR G292.0+1.8 of a young rapidly rotating pulsar and its associated pulsar wind nebula. Both the X-ray and radio luminosity of the pulsar wind nebula imply a spin-down energy-loss rate of E~1037 ergs s-1 for the still undetected pulsar. The pulsar candidate is 0.9′ from the geometric center of the SNR, which implies a transverse velocity of ~770(D/4.8 kpc)(t/1600 yr)-1 km s-1 assuming currently accepted values for the distance and age of G292.0+1.8.
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