MULTI-WAVELENGTH ANALYSIS OF THE GALACTIC SUPERNOVA REMNANT MSH 11-61A
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Auchettl-2015-MULTI-WAVELENGTH ANA.pdf
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Author(s)
Auchettl, Katie
Slane, Patrick
Castro, Daniel
Foster, Adam R.
Smith, Randall K.
Date Issued
August 2015
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Auchettl, Katie, Patrick Slane, Daniel Castro, Adam R. Foster, and Randall K. Smith. “MULTI-WAVELENGTH ANALYSIS OF THE GALACTIC SUPERNOVA REMNANT MSH 11-61A.” The Astrophysical Journal 810, no. 1 (August 27, 2015): 43. © 2015 The American Astronomical Society
Version
Final published version
Abstract
Due to its centrally bright X-ray morphology and limb brightened radio profile, MSH 11–61A (G290.1–0.8) is classified as a mixed morphology supernova remnant (SNR). H i and CO observations determined that the SNR is interacting with molecular clouds found toward the north and southwest regions of the remnant. In this paper we report on the detection of γ-ray emission coincident with MSH 11–61A, using 70 months of data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. To investigate the origin of this emission, we perform broadband modeling of its non-thermal emission considering both leptonic and hadronic cases and concluding that the γ-ray emission is most likely hadronic in nature. Additionally we present our analysis of a 111 ks archival Suzaku observation of this remnant. Our investigation shows that the X-ray emission from MSH 11–61A arises from shock-heated ejecta with the bulk of the X-ray emission arising from a recombining plasma, while the emission toward the east arises from an ionizing plasma.
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/810/1/43
