HAL : in2p3-00698357, version 1

DOI : 10.1088/0004-637X/749/2/131

Fiche détaillée

Récupérer au format BibTeX - EndNote - TEI - RefWorks -

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

(2012)

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

équipe(s) de recherche : ASTRO

Thème(s)

:

Physique/Astrophysique/Phénomènes cosmiques de haute energie Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie

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

in2p3-00698357, version 1

http://hal.in2p3.fr/in2p3-00698357

oai:hal.in2p3.fr:in2p3-00698357

Contributeur : Nathalie Martin <>

Déposé pour le compte de : Marianne LEMOINE GOUMARD <>

Soumis le : Mercredi 16 Mai 2012, 14:34:06

Dernière modification le : Mercredi 16 Mai 2012, 15:56:39