Towards gamma-ray astronomy with timing arrays

24th European Cosmic Ray Symposium

Tluczykont, M.^5 ; Astapov, I.^8 ; Barbashina, N.^8 ; Beregnev, S.^11 ; Bogdanov, A.^4 ; Bogorodskii, D.^1 ; Boreyko, V.^9 ; Brückner, M.^2 ; Budnev, N.^1 ; Chiavassa, A.^6 ; Chvalaev, O.^1 ; Dyachok, A.^1 ; Epimakhov, S.^5 ; Eremin, T.^11 ; Gafarov, A.^1 ; Gorbunov, N.^9 ; Grebenyuk, V.^9 ; Gress, O.^1 ; Gress, T.^1 ; Grinyuk, A.^9 ; Grishin, O.^1 ; Horns, D.^5 ; Ivanova, A.^1 ; Karpov, N.^11 ; Kalmykov, N.^11 ; Kazarina, Y.^1 ; Kindin, V.^4 ; Kirichkov, N.^1 ; Kiryuhin, S.^1 ; Kokoulin, R.^4 ; Kompaniets, K.^4 ; Konstantinov, E.^1 ; Korobchenko, A.^1 ; Korosteleva, E.^11 ; Kozhin, V.^11 ; Kunnas, M.^5 ; Kuzmichev, L.^11 ; Lenok, V.^1 ; Lubsandorzhiev, B.^10 ; Lubsandorzhiev, N.^11 ; Mirgazov, R.^1 ; Mirzoyan, R.^1,7 ; Monkhoev, R.^1 ; Nachtigall, R.^5 ; Pakhorukov, A.^1 ; Panasyuk, M.^11 ; Pankov, L.^1 ; Perevalov, A.^1 ; Petrukhin, A.^4 ; Platonov, V.^1 ; Poleschuk, V.^1 ; Popescu, M.^12 ; Popova, E.^11 ; Porelli, A.^3 ; Porokhovoy, S.^9 ; Prosin, V.^11 ; Ptuskin, V.^8 ; Romanov, V.^9 ; Rubtsov, G.^10 ; Rueger, M.^2,3 ; Rybov, E.^1 ; Samoliga, V.^1 ; Satunin, P.^10 ; Saunkin, A.^1 ; Savinov, V.^1 ; Semeney, Yu.^1 ; Shaibonov, B.^10 ; Silaev, A.^11 ; Silaev, A.^11 ; Skurikhin, A.^11 ; Slunecka, M.^9 ; Spiering, C.^3 ; Sveshnikova, L.^11 ; Tabolenko, V.^1 ; Tkachenko, A.^9 ; Tkachev, L.^9 ; Veslopopov, A.^1 ; Veslopopova, E.^1 ; Voronov, D.^1 ; Wischnewski, R.^3 ; Yashin, I.^4 ; Yurin, K.^4 ; Zagorodnikov, A.^1 ; Zirakashvili, V.^8 ; Zurbanov, V.^1

Institute of Applied Physics, Irkutsk State University, Irkutsk, Russia^1

Institute for Computer Science, Humboldt-University Berlin, Rudower Chaussee 25, Berlin

12489, Germany^2

DESY, Platanenallee 6, Zeuthen

15738, Germany^3

National Research Nuclear University, MEPhI (Moscow Engineering Physics Institute), Moscow, Russia^4

Institut für Experimentalphysik, Luruper Chaussee 149, Hamburg

22761, Germany^5

Dipartimento di Fisica Generale, Universiteta di Torino, INFN, Torino, Italy^6

Werner Heisenberg Institut, Föhringer Ring 6, München

80805, Germany^7

IZMIRAN, Troitsk, Moscow Region, Russia^8

Joint Institute for Nuclear Research, Joliot-Curie 6, Moscow region, Dubna

141980, Russia

(10) Institute for Nuclear Research, Russian Academy of Sciences, 60th October Anniversary st., 7a, Moscow

117312, Russia

(11) Skobeltsyn Institute for Nuclear Physics, Lomonosov Moscow State University, 1 Leninskie gory, Moscow

119991, Russia

(12) Institute of Space Science, Bucharest, Romania^9

关键词: Future perspectives;    Gamma ray emitter;    Gamma-ray astronomy;    Imaging air Cherenkov telescopes;    Large area telescopes;    Large effective areas;    Large viewing angle;    Sampling technique;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/632/1/012042/pdf
DOI  :  10.1088/1742-6596/632/1/012042

来源: IOP

【 摘 要 】

The gamma-ray energy regime beyond 10 TeV is crucial for the search for the most energetic Galactic accelerators. The energy spectra of most known gamma-ray emitters only reach up to few 10s of TeV, with 80 TeV from the Crab Nebula being the highest energy so far observed significantly. Uncovering their spectral shape up to few 100 TeV could answer the question whether some of these objects are cosmic ray Pevatrons, i.e. Galactic PeV accelerators. Sensitive observations in this energy range and beyond require very large effective detector areas of several 10s to 100 square-km. While imaging air Cherenkov telescopes have proven to be the instruments of choice in the GeV to TeV energy range, very large area telescope arrays are limited by the number of required readout channels per instrumented square-km (due to the large number of channels per telescope). Alternatively, the shower-front sampling technique allows to instrument large effective areas and also naturally provides large viewing angles of the instrument. Solely measuring the shower front light density and timing (hence timing- arrays), the primary particle properties are reconstructed on the basis of the measured lateral density function and the shower front arrival times. This presentation gives an overview of the technique, its goals, and future perspective.