A broadband study of the emission from the composite supernova remnant MSH 11-62 [electronic resource].
- Washington, D.C. : United States. Dept. of Energy, 2012.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy
- Physical Description:
- Article numbers 131 : digital, PDF file
- Additional Creators:
- SLAC National Accelerator Laboratory
United States. Department of Energy
United States. Department of Energy. Office of Scientific and Technical Information
- 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. Our observations suggest a relatively young system expanding into a low-density region. 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 also 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. Furthermore, 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.
- Published through SciTech Connect.
Astrophysical Journal 749 2 ISSN 0004-637X AM
Patrick Slane; John P. Hughes; Tea Temim; Romain Rousseau; Daniel Castro; Dillon Foight; B. M. Gaensler; Stefan Funk; Marianne Lemoine-Goumard; Joseph D. Gelfand; David A. Moffett; Richard G. Dodson; Joseph P. Bernstein.
- Funding Information:
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