Discovery of VHE γ-ray emission from the W49 region with H.E.S.S.

Brun, Francois; de Naurois, Mathieu; Hofmann, Werner; Carrigan, Svenja; Djannati-Atai, Arache; Ohm, Stefan

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Discovery of VHE γ-ray emission from the W49 region with H.E.S.S.

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Hofmann, Werner
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
for the H.E.S.S. Collaboration6;

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Carrigan, Svenja
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
for the H.E.S.S. Collaboration6;

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Ohm, Stefan
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
School of Physics & Astronomy, University of Leeds, UK;
Department of Physics & Astronomy, University of Leicester, UK;
for the H.E.S.S. Collaboration6;

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Citation

Brun, F., de Naurois, M., Hofmann, W., Carrigan, S., Djannati-Atai, A., & Ohm, S. (2011). Discovery of VHE γ-ray emission from the W49 region with H.E.S.S. Proceedings of Science, Texas2010: 201, 1-6.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0012-2F03-2

Abstract

TheW49 region hosts two bright radio sources: the star forming regionW49A and the supernova remnant W49B. The 10^6 M\odot Giant Molecular Cloud W49A is one of the most luminous giant radio HII regions in our Galaxy and hosts several active, high-mass star formation sites. The mixed-morphology supernova remnant W49B has one of the highest surface brightness in radio of all the SNRs of this class in our Galaxy and is one of the brightest ejecta-dominated SNRs in X-rays. Infrared observations evidenced that W49B is interacting with molecular clouds and Fermi recently reported the detection of a coincident bright, high-energy gamma-ray source. Observations by the H.E.S.S. telescope array resulted in the significant detection of VHE gamma-ray emission from theW49 region, compatible with VHE emission from the SNRW49B. The results, the morphology and the origin of the VHE emission are presented in themulti-wavelength context and the implications on the origin of the signal are discussed.