The development of the GAMMA-400 γ-ray telescope continues. The GAMMA-400 is designed to measure fluxes of γ-rays and the electron-positron cosmic-ray component possibly associated with annihilation or decay of dark matter particles; and to search for and study in detail discrete γ-ray sources, to measure the energy spectra of Galactic and extragalactic diffuse γ-rays, and to study γ-ray bursts and γ-rays from the active Sun. The energy range for measuring γ-rays and electrons (positrons) is from 100 MeV to 3000 GeV. For 100-GeV γ-rays, the γ-ray telescope has an angular resolution of ∼0.01°, an energy resolution of ∼1%, and a proton rejection factor of ∼5 × 105. The GAMMA-400 will be installed onboard the Russian Space Observatory.

The GAMMA-400 experiment: Status and prospects / Topchiev, N.P., Galper, A.M., Bonvicini, V., Adriani, O., Aptekar, R.L., Arkhangelskaja, I.V., Arkhangelskiy, A.I., Bergstrom, L., Berti, E., Bigongiari, G., Bobkov, S.G., Bogomolov, E.A., Boezio, M., Bongi, M., Bonechi, S., Bottai, S., Boyarchuk, K.A., Vacchi, A., Vannuccini, E., Vasilyev, G.I., et al.. - In: BULLETIN OF THE RUSSIAN ACADEMY OF SCIENCES. PHYSICS. - ISSN 1062-8738. - 79:3(2015), pp. 417-420. [10.3103/S1062873815030429]

The GAMMA-400 experiment: Status and prospects

Longo F.
Software
;
2015-01-01

Abstract

The development of the GAMMA-400 γ-ray telescope continues. The GAMMA-400 is designed to measure fluxes of γ-rays and the electron-positron cosmic-ray component possibly associated with annihilation or decay of dark matter particles; and to search for and study in detail discrete γ-ray sources, to measure the energy spectra of Galactic and extragalactic diffuse γ-rays, and to study γ-ray bursts and γ-rays from the active Sun. The energy range for measuring γ-rays and electrons (positrons) is from 100 MeV to 3000 GeV. For 100-GeV γ-rays, the γ-ray telescope has an angular resolution of ∼0.01°, an energy resolution of ∼1%, and a proton rejection factor of ∼5 × 105. The GAMMA-400 will be installed onboard the Russian Space Observatory.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11368/2965725
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