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The GeV Gamma-Ray Emission Detected by Fermi-LAT Adjacent to SNR Kesteven 41

Published online by Cambridge University Press:  17 October 2017

Bing Liu ,
Yang Chen ,
Xiao Zhang ,
Gao-Yuan Zhang ,
Yi Xing  and
Thomas G. Pannuti
Bing Liu
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China
Yang Chen
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China
Xiao Zhang
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China
Gao-Yuan Zhang
Affiliation:
Department of Astronomy, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China
Yi Xing
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Thomas G. Pannuti
Affiliation:
Space Science Center, Department of Earth and Space Sciences, Morehead State University, 235 Martindale Drive, Morehead, KY 40351, USA
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Abstract

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Gamma-ray observations for Supernova remnant (SNR)-molecular cloud (MC) association systems play an important role in the research on the acceleration and propagation of cosmic-ray protons. Through the analysis of 5.6 years of Fermi-Large Area Telescope observation data, here we report on the detection of a gamma-ray emission source near the SNR Kesteven 41 with a significance of 24σ in 0.2–300 GeV. The best-fit location of the gamma-ray source is consistent with the MC with which the SNR interacts. Several hypotheses including both leptonic and hadronic scenarios are considered to investigate the origin of these gamma-rays. The gamma-ray emission can be naturally explained by the decay of neutral pions produced via the collision between high energy protons accelerated by the shock of Kesteven 41 and the adjacent MC. The electron energy budget would be too high for the SNR if the gamma-rays were produced via inverse Compton (IC) scattering off the Cosmic Microwave Background (CMB) photons.

Keywords

acceleration of particlesgamma rays: observationssupernova remnantsISM: individual (Kes 41)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 310 - 315
Copyright
Copyright © International Astronomical Union 2017 

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