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Chandra Study of the Central Object Associated with the Supernova Remnant MSH 11–62

Published online by Cambridge University Press:  19 July 2016

Ilana Harrus ,
Joseph P. Bernstein ,
Patrick O. Slane ,
Bryan Gaensler ,
John P. Hughes ,
David Moffett  and
Richard Dodson
Ilana Harrus
Affiliation:
Goddard Space Flight Center, Greenbelt, MD 20771, USA
Joseph P. Bernstein
Affiliation:
University of Michigan, Ann Arbor, MI 48109, USA
Patrick O. Slane
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
Bryan Gaensler
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
John P. Hughes
Affiliation:
Rutgers University, Piscataway, NJ 08854, USA
David Moffett
Affiliation:
Furman University, Greenville, SC 29613, USA
Richard Dodson
Affiliation:
Japan Aerospace Exploration Agency (JAXA), Kanagawa, 229-8510, Japan

Abstract

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We present results from our analysis of Chandra data on the supernova remnant MSH 11–62 (also known as G291.0−0.1). Our previous ASCA analysis showed that MSH 11–62 is most likely a composite remnant whose strong non-thermal emission is powered by a compact object, most probably a pulsar. The present analysis confirms in a spectacular fashion the earlier detection of a compact source. The Chandra data reveal a small region with a hard non-thermal spectrum located at the tip of the central radio emission seen in data taken at the Australia Telescope Compact Array (ATCA). This source is likely the young rapidly rotating neutron star powering the synchrotron nebula in MSH 11–62. Compared to other young rotation-powered pulsars the Chandra specrum of MSH 11–62 implies an energy loss rate of Ė ∼ 5 × 1036 ergs s−1.

Type
Part 4: Pulsar Wind Nebulae and Their Environments
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 203 - 206
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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