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The H.E.S.S. view of the Milky Way in TeV light

Published online by Cambridge University Press:  17 August 2012

Christoph Deil
Christoph Deil*
Affiliation:
Max-Planck-Institute for Nuclear Physics, P.O. Box 103980, 69029 Heidelberg, Germany email: Christoph.Deil@mpi-hd.mpg.de
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Abstract

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Since 2003 the H.E.S.S. collaboration has been operating an array of four imaging Cherenkov telescopes in the Khomas Highlands of Namibia. H.E.S.S. can detect gamma rays in the energy range 100 GeV to 100 TeV, has a large field of view (5 degree), good angular resolution (0.1 degree), energy resolution (15%) and sensitivity (a 1% Crab flux point source is detected at 5 sigma significance in 25 h). About half of the available observing time has been spent on the Milky Way, either in scan mode or on individual sources, resulting in the detection of more than 60 Galactic TeV sources. In this talk the two most numerous source classes will be discussed, pulsar wind nebulae and supernova remnants. For the identification and understanding of the TeV emission seen by H.E.S.S. additional measurements of non-thermal emission, mainly in the radio, X-ray and lower-energy gamma-ray bands, are critical. Since August 2008 the Fermi Large Area Telescope has been scanning the whole sky in the energy range from 20 MeV to more than 300 GeV and has detected about 200 Galactic sources as well as diffuse emission from the Milky Way. This talk will give an overview of Galactic H.E.S.S. observations in the multi-wavelength context, with a focus on Fermi.

Keywords

surveysgamma rays: observationscosmic raysGalaxy: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 365 - 370
Copyright
Copyright © International Astronomical Union 2012

References

Abdo, A. A. and Fermi LAT Collaboration 2011, ArXiv e-prints, 1103.5727Google Scholar
Acero, F. et al. 2010, MNRAS, 402, 1877Google Scholar
Aharonian, F. et al. 2007, ApJ, 661, 236Google Scholar
Becherini, Y. et al. 2010, American Institute of Physics Conference Series, 1085, 738Google Scholar
Berge, D., Funk, S., & Hinton, J. 2007, A&A, 466, 1219Google Scholar
Brun, F. et al. 2011, ArXiv e-prints, 1104.5003Google Scholar
Daugherty, J. K. & Harding, A. K. 1982, ApJ, 252, 337CrossRefGoogle Scholar
The Fermi-LAT Collaboration 2011, ArXiv e-prints, 1108.1435Google Scholar
Gaensler, B. M. & Slane, P. O. 2006, ARA&A, 44, 17Google Scholar
Gast, H. et al. 2011, Proc. 32nd ICRC, Beijing, in pressGoogle Scholar
Horns, D. et al. 2007, Ap&SS, 309, 189Google Scholar
Meyer, M., Horns, D. & Zechlin, H. 2010, MNRAS, 523, A2.Google Scholar
Morlino, G. & Caprioli, D. 2011, ArXiv e-prints, 1105.6342Google Scholar
Ohm, S., van Eldik, C., & Egberts, K. 2009, Astroparticle Physics, 31, 383CrossRefGoogle Scholar