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Characteristics of the GAMMA-400 gamma-ray telescope for searching for dark matter signatures

  • Proceedings of the 32nd All-Russia Conference on Cosmic Rays (Moscow, July 2012)
  • Published:
Bulletin of the Russian Academy of Sciences: Physics Aims and scope

Abstract

The GAMMA-400 gamma-ray telescope currently under development is designed to measure fluxes of gamma rays and electron-positron cosmic-ray components, which could be associated with the annihilation or decay of dark matter particles, and to survey in detail the celestial sphere in order to search for and investigate discrete gamma-ray sources; to measure the energy spectra of Galactic and extragalactic dif- fuse gamma-ray emissions; and to study gamma-ray bursts and the gamma-ray emissions of active Sun. The GAMMA-400 energy range is 100 MeV to 3000 GeV. The gamma-ray telescope has an angular resolution of ∼0.01°, an energy resolution of ∼1%, and a proton rejection factor of ∼106. The GAMMA-400 will be installed on Russia’s Navigator space platform. Observations are planned to commence in 2018.

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Correspondence to A. M. Galper.

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Original Russian Text © A.M. Galper, O. Adriani, R.L. Aptekar, I.V. Arkhangelskaja, A.I. Arkhangelskiy, M. Boezio, V. Bonvicini, K.A. Boyarchuk, A. Vacchi, E. Vannuccini, Yu.V. Gusakov, N. Zampa, V.G. Zverev, V.N. Zirakashvili, V.A. Kaplin, V.A. Kachanov, A.A. Leonov, F. Longo, E.P. Mazets, P. Maestro, P. Marrocchesi, I.A. Mereminskiy, V.V. Mikhailov, A.A. Moiseev, E. Mocchiutti, N. Mori, I.V. Moskalenko, P.Yu. Naumov, P. Papini, P. Picozza, V.G. Rodin, M.F. Runtso, R. Sparvoli, P. Spillantini, S.I. Suchkov, M. Tavani, N.P. Topchiev, M.I. Fradkin, M.D. Kheymits, Y.T. Yurkin, 2013, published in Izvestiya Rossiiskoi Akademii Nauk. Seriya Fizicheskaya, 2013, Vol. 77, No. 11, pp. 1605–1608.

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Galper, A.M., Adriani, O., Aptekar, R.L. et al. Characteristics of the GAMMA-400 gamma-ray telescope for searching for dark matter signatures. Bull. Russ. Acad. Sci. Phys. 77, 1339–1342 (2013). https://doi.org/10.3103/S1062873813110105

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  • DOI: https://doi.org/10.3103/S1062873813110105

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