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A BROADBAND STUDY OF THE EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 11-62

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Patrick Slane1, John P. Hughes2, Tea Temim3, Romain Rousseau4, Daniel Castro1, Dillon Foight1, B. M. Gaensler5, Stefan Funk6, Marianne Lemoine-Goumard4, Joseph D. Gelfand7, David A. Moffett8, Richard G. Dodson9, and Joseph P. Bernstein10,11

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MSH 11-62 (G291.0-0.1) is a composite supernova remnant for which radio and X-ray observations have identified the remnant shell as well as its central pulsar wind nebula. The observations suggest a relatively young system expanding into a low-density region. Here, we present a study of MSH 11-62 using observations with the Chandra, XMM -Newton, and Fermi observatories, along with radio observations from the Australia Telescope Compact Array. We identify a compact X-ray source that appears to be the putative pulsar that powers the nebula, and show that the X-ray spectrum of the nebula bears the signature of synchrotron losses as particles diffuse into the outer nebula. Using data from the Fermi Large Area Telescope, we identify γ-ray emission originating from MSH 11-62. With density constraints from the new X-ray measurements of the remnant, we model the evolution of the composite system in order to constrain the properties of the underlying pulsar and the origin of the γ-ray emission.


Keywords

ISM: individual objects (MSH-11-62); ISM: supernova remnants; radiation mechanisms: non-thermal; stars: neutron


Dates

Issue 2 (2012 April 20)

Received 2011 October 14, accepted for publication 2012 February 5

Published 2012 March 30

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