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Comptes Rendus Physique
Volume 16, n° 6-7
pages 587-599 (août 2015)
Doi : 10.1016/j.crhy.2015.07.003
Introduction to high-energy gamma-ray astronomy
Introduction à l'astronomie gamma de haute énergie
 

Bernard Degrange , Gérard Fontaine
 Laboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Université Paris-Saclay, 91128 Palaiseau cedex, France 

Corresponding authors.
Abstract

The present issue is the first of a two-volume review devoted to gamma-ray astronomy above 100 MeV, which has witnessed considerable progress over the last 20 years. The motivations for research in this area are explained, the follow-on articles of these two issues are introduced and a brief history of the field is given.

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Résumé

Le présent numéro est le premier de deux volumes consacrés à l'astronomie gamma de haute énergie au-dessus de 100 MeV, qui a considérablement progressé au cours des vingt dernières années. Cet article expose les motivations à la base de cette recherche, présente les articles de ces deux fascicules et fournit une brève introduction historique au domaine.

The full text of this article is available in PDF format.

Keywords : Cosmic rays, Non-thermal radiation, High-energy gamma rays, Space-borne detectors, Ground-based detectors

Mots-clés : Rayons cosmiques, Rayonnement non thermique, Rayons gamma de haute énergie, Détecteurs en satellite, Détecteurs au sol


1  Note that γ rays can also undergo hadronic interactions, e.g.,  .
2  In the notation of radio-astronomy, the SED takes the form  , in which ν is the photon frequency and   is the power received per unit area and frequency.
3  In some cases, such processes are associated with extended objects resulting from many supernova explosions or stellar winds. Such a “superbubble” has recently been observed in the Large Magellanic Cloud [[7]].
4  Note that the effective detection area is not related to the size of the mirror, the latter being relevant for the detection threshold.


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