SLANE, P.; P. HUGHES, J.; TEMIM, T.; ROUSSEAU, R.; CASTRO, D.L; FOIGHT, D.; M. GAENSLER, B.; FUNK, S.; LEMOINE-GOUMARD, M.; D. GELFAND, J.; MOFFETT, D.A.; G. DODSON, R.; P. BERNSTEIN, J.

doi:10.1088/0004-637X/749/2/131

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The Astrophysical Journal. 2012, vol. 749, p. 131

American Astronomical Society

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MSH 11-62 (G291.1-0.9) 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 (ATCA). 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 LAT, we identify gamma-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 gamma-ray emission.< Réduire

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ISM: supernova remnants

radiation mechanisms: non-thermal

stars: neutron

ISM: individual objects (MSH-11-62)

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A Broadband Study of the Emission from the Composite Supernova Remnant MSH 11-62

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