Fermi LAT Observations of Supernova Remnants Interacting with Molecular Clouds: W41, MSH 17-39, and G337.0-0.1

Abstract

We report the detection of gamma-ray emission coincident with three supernova remnants (SNRs) using data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. W41, MSH 17-39, and G337.0-0.1 are SNRs known to be interacting with molecular clouds, as evidenced by observations of hydroxyl (OH) maser emission at 1720 MHz in their directions and other observational information. SNR shocks are expected to be sites of cosmic ray acceleration, and clouds of dense material can provide effective targets for production of gamma-rays from neutral pion-decay. The observations reveal unresolved sources in the direction of G337.0-0.1, and MSH 17-39, and an extended source coincident with W41. We model their broadband emission (radio to gamma-ray) using a simple one-zone model, and after considering scenarios in which the MeV-TeV sources originate from either neutral pion-decay or leptonic emission, we conclude that the gamma-rays are most likely produced through the hadronic channel.

9 pages, 11 figures, accepted for publication in ApJ

References in corpus (7)

• Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
• Parameterization of Gamma, e^+/- and Neutrino Spectra Produced by p-p Interaction in Astronomical Environment
• Observations of the young supernova remnant RX J1713.7-3946 with the Fermi Large Area Telescope
• Measuring the cosmic ray acceleration efficiency of a supernova remnant
• The Distances of SNR W41 and overlapping HII regions
• VLA and XMM-Newton observations of the SNR W41/TeV Gamma-ray source HESS J1834-087
• Evidence of a Hadronic Origin for the TeV Source J1834-087

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