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The Astrophysical Journal 749 (2012) 131
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

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.
1:  CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
Physics/Astrophysics/High Energy Astrophysical Phenomena

Sciences of the Universe/Astrophysics/High Energy Astrophysical Phenomena
ISM: individual objects (MSH-11-62) - ISM: supernova remnants - radiation mechanisms: non-thermal - stars: neutron