Towards gamma-ray astronomy with timing arraysстатья
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Дата последнего поиска статьи во внешних источниках: 10 февраля 2016 г.
Авторы:Tluczykon M.,
Astapov I.,
Barbashina N.,
Beregnev S.,
Bogdanov A.,
Bogorodskii D.,
Boreyko V.,
Brückner M.,
Budnev N.,
Chiavassa A.,
Chvalaev O.,
Dyachok A.,
Epimakhov S.,
Eremin T.,
Gafarov A.,
Gorbunov N.,
Grebenyuk V.,
Gress O.,
Gress T.,
Grinyuk A.,
Grishin O.,
Horns D.,
Ivanova A.,
Karpov N.,
Kalmykov N.,
Kazarina Y.,
Kindin V.,
Kirichkov N.,
Kiryuhin S.,
Kokoulin R.,
Kompaniets K.,
Konstantinov E.,
Korobchenko A.,
Korosteleva E.,
Kozhin V.,
Lenok V.,
Lubsandorzhiev B.,
Lubsandorzhiev N.,
Mirgazov R.,
Mirzoyan R.,
Monkhoev R.,
Nachtigall R.,
Pakhorukov A.,
Panasyuk M.,
Pankov L.,
Perevalov A.,
Petrukhin A.,
Platonov V.,
Poleschuk V.,
Popescu M.,
Popova E.G.,
Porelli A.,
Porokhovoy S.,
Prosin V.,
Ptuskin V.,
Romanov V.,
Rubtsov G.,
Rueger M.,
Rybov E.,
Samoliga V.,
Satunin P.,
Saunkin A.,
Savinov V.,
Semeney Yu,
(junior) Shaibonov B.,
Silaev A.,
(junior) Silaev A.,
Skurikhin A.,
Slunecka M.,
Spiering C.,
Sveshnikova L.,
Tabolenko V.,
Tkachenko A.,
Tkachev L.,
Veslopopov A.,
Veslopopova E.,
Voronov D.,
Wischnewski R.,
Yashin I.,
Yurin K.,
Zaorodnikov A.,
Zirakashvili V.,
Zurbanov V.
Аннотация: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 timingarrays),
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.