HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56
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Temim-2013-High-energy emission.pdf
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Author(s)
Temim, Tea
Slane, Patrick
Castro, Daniel
Plucinsky, Paul P.
Gelfand, Joseph D.
Dickel, John R.
Date Issued
April 2013
Journal
Astrophysical Journal
Publisher
IOP Publishing
Citation
Temim, Tea, Patrick Slane, Daniel Castro, Paul P. Plucinsky, Joseph Gelfand, and John R. Dickel. “ HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-5 6 .” The Astrophysical Journal 768, no. 1 (April 15, 2013): 61. © 2013 The American Astronomical Society
Version
Final published version
Abstract
MSH 15-56 (G326.3–1.8) is a composite supernova remnant (SNR) that consists of an SNR shell and a displaced pulsar wind nebula (PWN) in the radio. We present XMM-Newton and Chandra X-ray observations of the remnant that reveal a compact source at the tip of the radio PWN and complex structures that provide evidence for mixing of the supernova (SN) ejecta with PWN material following a reverse shock interaction. The X-ray spectra are well fitted by a non-thermal power-law model whose photon index steepens with distance from the presumed pulsar, and a thermal component with an average temperature of 0.55 keV. The enhanced abundances of silicon and sulfur in some regions, and the similar temperature and ionization timescale, suggest that much of the X-ray emission can be attributed to SN ejecta that have either been heated by the reverse shock or swept up by the PWN. We find one region with a lower temperature of 0.3 keV that appears to be in ionization equilibrium. Assuming the Sedov model, we derive a number of SNR properties, including an age of 16,500 yr. Modeling of the γ-ray emission detected by Fermi shows that the emission may originate from the reverse shock-crushed PWN.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637X/768/1/61
