Magic observations of very high energy γ-rays from HESS J1813-178

  • J. Albert
  • , E. Aliu
  • , H. Anderhub
  • , P. Antoranz
  • , A. Armada
  • , M. Asensio
  • , C. Baixeras
  • , J. A. Barrio
  • , M. Bartel
  • , H. Bartko
  • , D. Bastieri
  • , R. Bavikadi
  • , W. Bednarek
  • , K. Berger
  • , C. Bigongiari
  • , A. Biland
  • , E. Bisesi
  • , O. Blanch
  • , R. K. Bock
  • , T. Bretz
  • I. Britvitch, M. Camara, A. Chilingarian, S. Ciprini, J. A. Coarasa, S. Commichau, J. L. Contreras, J. Cortina, V. Curtev, V. Danielyan, F. Dazzi, A. De Angelis, R. De Los Reyes, B. De Lotto, E. Domingo-Santamaria, D. Dorner, M. Doro, M. Errando, M. Fagiolini, D. Ferenc, E. Fernández, R. Firpo, J. Flix, M. V. Fonseca, L. Font, N. Galante, M. Garczarczyk, M. Gaug, J. Gebauer, M. Giller, F. Goebel, D. Hakobyan, M. Hayashida, T. Hengstebeck, D. Höhne, J. Hose, P. Jacon, O. Kalekin, D. Kranich, A. Laille, T. Lenisa, P. Liebing, E. Lindfors, F. Longo, M. López, J. López, E. Lorenz, F. Lucarelli, P. Majumdar, G. Maneva, K. Mannheim, M. Mariotti, M. Martínez, K. Mase, D. Mazin, C. Merck, M. Merck, M. Meucci, M. Meyer, J. M. Miranda, R. Mirzoyan, S. Mizobuchi, A. Moralejo, K. Nilsson, E. Oña-Wilhelmi, R. Orduña, N. Otte, I. Oya, D. Paneque, R. Paoletti, M. Pasanen, D. Pascoli, F. Pauss, N. Pavel, R. Peona, L. Peruzzo, A. Piccioli, E. Prandini, J. Rico

Research output: Contribution to journalArticlepeer-review

47 Scopus citations

Abstract

Recently, the HESS collaboration has reported the detection of γ-ray emission above a few hundred GeV from eight new sources located close to the Galactic plane. The source HESS J1813-178 has sparked particular interest, as subsequent radio observations imply an association with supernova remnant G12.82-0.02. Triggered by the detection in very high energy γ-rays, a positionally coincident source has also been found in INTEGRAL and ASCA data. In this Letter we present MAGIC observations of HESS J1813-178, resulting in the detection of a differential γ-ray flux consistent with a hard-slope power law, described as dNγ/(dA dt dE) = (3.3 ± 0.5) × 10-12(E/TeV)-2.1±0.2 cm-2s -1TeV-1. We briefly discuss the observational technique used and the procedure implemented for the data analysis, and we put this detection in the perspective of multifrequency observations.

Original languageEnglish
Pages (from-to)L41-L44
JournalAstrophysical Journal
Volume637
Issue number1 II
DOIs
StatePublished - Jan 20 2006

Keywords

  • Acceleration of particles
  • Gamma rays: observations
  • Supernova remnants

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