Статья посвящена моделированию и анализу данных, регистрируемых установкой TAIGA-IACT в стереорежиме. Установка будет включать 5 атмосферных черенковских телескопов с углом обзора 9.6°. В настоящее время в составе установки имеются 3 телескопа, разнесенных на сравнительно большие расстояния друг от друга (от 320 до 500 м). Эффективная площадь установки при этом достигает 0.6 км2, что позволяет за разумное время наблюдения (300–400 ч) проводить статистически значимые наблюдения слабых источников гамма-излучения в энергетической области выше 10 ТэВ. Описана процедура моделирования Монте-Карло регистрируемых телескопами адронов и гамма-квантов, а также методика восстановления параметров широких атмосферных ливней, таких как направление прихода события, положение оси, глубина максимума развития ливня и энергия первичной частицы. Для решения задачи гамма-адронного разделения получены оптимальные критерии отбора гамма-квантов, регистрируемых в стереорежиме, и рассчитана эффективная площадь установки.
The paper is devoted to the modeling and analysis of data detected by the TAIGA-IACT installation in the stereo mode. Five Imaging Atmospheric Cherenkov Telescopes (IACT) with a viewing angle of 9.6° are expected to be included in the installation. Today there are three telescopes spaced far apart (from 320 to 500 m) in the installation. The effective area of the installation is as large as 0.6 km2; therefore, it is possible to conduct statistically significant measurements of weak γ-ray sources in the energy range above 10 TeV over a reasonable observation time (300–400 h). The Monte Carlo procedure for simulating the hadrons and γ-rays detected by the telescopes is described as is the procedure for reconstructing the parameters of extensive air showers, such as the arrival direction of an event, the axis position, the depth of the maximum of shower development (Xmax), and the primary-particle energy. In order to solve the problem of γ-hadron separation, the criteria for selecting γ-rays detected in the stereo mode have been optimized and the effective area of the installation has been calculated.
The 1-cubic km deep Baikal-GVD underwater Cherenkov detector, a new-generation neutrino telescope, is now being deployed in Lake Baikal. The telescope’s status is described and the first physical results from its operation are presented.
Baikal-GVD is a next generation, kilometer-scale neutrino telescope under construction in Lake Baikal. It is designed to detect astrophysical neutrino fluxes at energies from a few TeV up to 100 PeV. GVD is formed by multi-megaton subarrays (clusters). The array construction started in 2015 by deployment of a reduced-size demonstration cluster named "Dubna" . The first cluster in it’s baseline configuration was deployed in 2016, the second in 2017 and the third in 2018. The full-scale GVD will be an array of ~10.000 light sensors with an instrumented volume about of 2 cubic km. The first phase (GVD-1) is planned to be completed by 2020-2021. It will comprise 8 clusters with 2304 light sensors in total. We describe the design of Baikal-GVD and present selected results obtained in 2015 - 2017.