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Conference Paper

The W49 region as seen by H.E.S.S.

MPS-Authors
http://pubman.mpdl.mpg.de/cone/persons/resource/persons31147

Brun,  Francois
Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, Palaiseau, France;
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons30605

Hofmann,  Werner
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons30367

Carrigan,  Svenja
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons30861

Ohm,  Stefan
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
School of Physics & Astronomy, University of Leeds, UK;

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Citation

Brun, F., de Naurois, M., Hofmann, W., Carrigan, S., Djannati-Atai, A., Ohm, S., et al. (2011). The W49 region as seen by H.E.S.S. Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, 545-548.


Cite as: http://hdl.handle.net/11858/00-001M-0000-000F-4A34-4
Abstract
The W49 region hosts a star forming region (W49A) and a supernova remnant interacting with molecular clouds (W49B). The 10^6 M_{sun} Giant Molecular Cloud W49A is one of the most luminous giant radio H II region in our Galaxy and hosts several active, high-mass star formation sites. The mixed-morphology supernova remnant W49B has one of the highest radio surface brightness of all the SNRs of this class in our Galaxy. 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 the W49 region, compatible with gamma-ray emission from the SNR W49B. The results, the morphology and the origin of the VHE gamma-ray emission are presented in the multi-wavelength context and the implications on the origin of the signal are discussed.