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A Broadband Study of the Emission from the Composite Supernova Remnant MSH 11-62
Slane P., P. Hughes J., Temim T., Rousseau R., Castro D. et al
The Astrophysical Journal 749 (2012) 131 - http://hal.in2p3.fr/in2p3-00698357
Physique/Astrophysique/Phénomènes cosmiques de haute energie
Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie
A Broadband Study of the Emission from the Composite Supernova Remnant MSH 11-62
P. Slane, J. P. Hughes, T. Temim, R. Rousseau1, D.L Castro, D. Foight, B. M. Gaensler, S. Funk, M. Lemoine-Goumard1, J. D. Gelfand, D. A. Moffett, R. G. Dodson, J. P. Bernstein
1 :  CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
http://www.cenbg.in2p3.fr/
CNRS : UMR5797 – IN2P3 – Université Sciences et Technologies - Bordeaux I
Chemin du Solarium - BP 120 - 33175 Gradignan Cedex
France
ASTRO
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.

Articles dans des revues avec comité de lecture
2012
The Astrophysical Journal
749
131

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