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HiSCORE is a non-imaging wide-angle Cherenkov array for the detection of extensive air showers induced by ultrahigh energy gamma-rays above 10 TeV and cosmic ray studies above 100 TeV. In October 2013 a 9-station engineering array has been deployed in Tunka valley. For HiSCORE-9, two DAQ systems are being used. The second system is a DRS4 based acquisition system with WhiteRabbit integrated time synchronization. We present the first results on the amplitude calibration from the data of this DAQ system.

The Tunka-HiSCORE detector follows the concept of a non-imaging wide-angle EAS Cherenkov array, designed to search for γ-ray sources above 10 TeV and to investigate the spectrum and composition of cosmic-rays above 100 TeV. A prototype array with 9 stations has been deployed in October 2013 at the site of the Tunka experiment in Russia. We describe design and performance of the array data acquisition system DAQ-2, focusing on its timing system based on the White Rabbit technology for sub-nsec time-synchronization over ethernet. First results of EAS arrival direction reconstruction, compared with MC simulations, and tests with artifical light sources verify an excellent performance of the system.

The design for the TAIGA-HiSCORE array, a part of the TAIGA Gamma Ray Observatory, is considered. The observatory is being constructed in the Tunka Valley, 50 km from Lake Baikal. Preliminary results obtained using the first 28 optical stations of the array are presented.

The Tunka Advanced Instrument for Gamma- and cosmic-ray Astronomy (TAIGA) is a multicomponent experiment for the measurement of TeV to PeV gamma- and cosmic rays. Our goal is to establish a novel hybrid direct air shower technique, sufficient to access the energy domain of the long-sought Pevatrons. The hybrid air Cherenkov light detection technique combines the strengths of the HiSCORE shower front sampling array, and two \\(\\thicksim\\)4 m class, \\(\\sim\\)9.6 deg field of view Imaging Air Cherenkov Telescopes (IACTs). The HiSCORE array provides good angular and shower core position resolution, while the IACTs provide the image shape and orientation for gamma-hadron separation. In future, an additional muon detector will be used for hadron tagging at \\(\\ge\\) 100 TeV energies. Here, only data from the first IACT of the TAIGA experiment are used. A random forest algorithm was trained using Monte Carlo (MC) simulations and real data, and applied to 85 h of selected observational data tracking the Crab Nebula at a mean zenith angle of 33.5 deg, resulting in a threshold energy of 6 TeV for this dataset. The analysis was performed using the gammapy package. A total of 163.5 excess events were detected, with a statistical significance of 8.5 sigma. The observed spectrum of the Crab Nebula is best fit with a power law above 6 TeV with a flux normalisation of \\((3.20\\pm0.42)\\cdot10^{-10} TeV^{-1} cm^{-2} s^{-1})\\) at a reference energy of 13 TeV and a spectral index of \\(-2.74\\pm0.16\\).

The paper is a script of a lecture given at the ISAPP-Baikal summer school in 2018. The lecture gives an overview of the Tunka Advanced Instrument for cosmic rays and Gamma Astronomy (TAIGA) facility including historical introduction, description of existing and future setups, and outreach and open data activities.

The paper is a script of a lecture given at the ISAPP-Baikal summer school in 2018. The lecture gives an overview of the Tunka Advanced Instrument for cosmic rays and Gamma Astronomy (TAIGA) facility including historical introduction, description of existing and future setups, and outreach and open data activities.

The TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) experiment aims to establish a new technology for ground-based gamma-astronomy by combining both Cherenkov imaging and non-imaging timing techniques. By detecting cosmic rays (CR) above 100 TeV and gamma-rays in the energy range from 10 TeV up to several PeV, TAIGA will address CR composition and spectral measurements in the Galactic/extragalactic transition region, and the origin of CRs by searching for galactic PeVatrons.The main topic of this work is TAIGA-HiSCORE, the wide-aperture air Cherenkov timing array. The focus is on precision shower arrival direction reconstruction, that is achieved by (1) sub-nsec time-synchronization between all array stations based on a dedicated hardware timing system, and (2) a newly developed time calibration procedure that minimizes mispointing. The performance is verified using events originating fromextensive air shower (EAS) and from a LIDAR laser beam from the International Space Station (ISS).First,we analyse HiSCORE 9 data collected with a data acquisition system based on the White Rabbit (WR) timing system. The station time offset calibration is obtained using a LED light source signal and allows a precise arrival direction reconstruction of the detected EAS data. The analysis of both EAS and LED data allows to verify the sub-nsec time synchronization of the WR system.In the analysis of the HiSCORE 28 data, taken from 2015–2018, we address the problem of achieving an easy-to-perform array time calibration for large area ground-based Cherenkov detectors. The intrinsic limits of the \"self-time calibration method\", which uses EAS to estimate the time offsets, are discussed. A new \"hybrid\" calibration method is developed, which makes use of EAS data, and requires direct LED calibration of only a few array stations. The efficiency and stability of the hybrid method has been tested using MC simulations. As for HiS9, the analysis of both EAS and LED data allow to verify the sub-nsec time synchronization of the timing system. Finally, the \"chessboard\" method is applied on the reconstructed data to obtain a MC-independent estimation of the detector angular resolution. It is found to be 0.4° at threshold (∼50 TeV) and ≤ 0.2° above 100 TeV.A serendipitous discoverywas made in thiswork: events that originate fromthe CATS-LIDAR on-board the ISS were found in the HiSCORE 28 data sample. After understanding their main characteristics, these \"ISS-events\", which make up a quasi-point-source, are used to verify the array time synchronization, the correctness of the array time calibration and event reconstruction, and the detector absolute angular pointing (≤ 0.1°). This absolute pointing calibration is particularly important since a strong gamma point source has not yet been detected by the TAIGA-HiSCORE 28 detector.The final part of the work presents a first approach to a wide aperture point source analysis, developed for the TAIGA-HiSCORE detector in stand-alone operation. The analysis is tested on the three years HiS28 data sample, with a focus on the region around the Crab Nebula. After showing the preliminary results, the limits of the current implementation and improvements to increase the detection potential are discussed.

ULTRASAT (ULtra-violet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform a deep time-resolved all-sky survey in the near-ultraviolet (NUV) spectrum. The science objectives are the detection of counterparts to short-lived transient astronomical events such as gravitational wave sources and supernovae. The mission is led by the Weizmann Institute of Science and is planned for launch in 2026 in collaboration with the Israeli Space Agency and NASA. DESY will provide the UV camera, composed by the detector assembly located in the telescope focal plane and the remote electronics unit. The camera is composed out of four back-metallized CMOS Image Sensors (CIS) manufactured in the 4T, dual gain Tower process. As part of the radiation qualification of the camera, Single Event Effect (SEE) testing has been performed by irradiating the sensor with heavy ions at the RADEF, Jyvaskyla facility. Preliminary results of both Single Event Upset (SEU) and Single Event Latch-up (SEL) occurrence rate in the sensor are presented. Additionally, an in-orbit SEE rate simulation has been performed in order to gain preliminary knowledge about the expected effect of SEE on the mission.

The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is a space-borne near UV telescope with an unprecedented large field of view (200 sq. deg.). The mission, led by the Weizmann Institute of Science and the Israel Space Agency in collaboration with DESY (Helmholtz association, Germany) and NASA (USA), is fully funded and expected to be launched to a geostationary transfer orbit in Q2/3 of 2025. With a grasp 300 times larger than GALEX, the most sensitive UV satellite to date, ULTRASAT will revolutionize our understanding of the hot transient universe, as well as of flaring galactic sources. We describe the mission payload, the optical design and the choice of materials allowing us to achieve a point spread function of ~10arcsec across the FoV, and the detector assembly. We detail the mitigation techniques implemented to suppress out-of-band flux and reduce stray light, detector properties including measured quantum efficiency of scout (prototype) detectors, and expected performance (limiting magnitude) for various objects.

Lori-Ann Touchette and Paolo Porelli unveil a new international centre for ceramics in Rome.