TY - JOUR
T1 - Fermi-lat observations of supernova remnants interacting with molecular clouds
T2 - W41, MSH 17-39, and G337.7-0.1
AU - Castro, Daniel
AU - Slane, Patrick
AU - Carlton, Ashley
AU - Figueroa-Feliciano, Enectali
PY - 2013/9/1
Y1 - 2013/9/1
N2 - We report the detection of γ-ray emission coincident with three supernova remnants (SNRs) using data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. W41, G337.7-0.1, and MSH 17-39 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 γ-rays from π0-decay. The observations reveal unresolved sources in the direction of G337.7-0.1 and MSH 17-39 and an extended source coincident with W41. We model their broadband emission (radio to γ-ray) using a simple one-zone model, and after considering scenarios in which the MeV-TeV sources originate from either π0-decay or leptonic emission, we conclude that the γ-rays are most likely produced through the hadronic channel.
AB - We report the detection of γ-ray emission coincident with three supernova remnants (SNRs) using data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. W41, G337.7-0.1, and MSH 17-39 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 γ-rays from π0-decay. The observations reveal unresolved sources in the direction of G337.7-0.1 and MSH 17-39 and an extended source coincident with W41. We model their broadband emission (radio to γ-ray) using a simple one-zone model, and after considering scenarios in which the MeV-TeV sources originate from either π0-decay or leptonic emission, we conclude that the γ-rays are most likely produced through the hadronic channel.
KW - ISM: individual objects (W41, MSH 17-39, G337.7-0.1)
KW - ISM: supernova remnants
KW - acceleration of particles
KW - cosmic rays
KW - gamma rays: ISM
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U2 - 10.1088/0004-637X/774/1/36
DO - 10.1088/0004-637X/774/1/36
M3 - Article
AN - SCOPUS:84882790768
SN - 0004-637X
VL - 774
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 36
ER -