The main goal of the TUS experiment was to search for and study ultra high-energy cosmic rays with energies E > 70 EeV. The TUS detector registered a number of unusual events, the origin of which is unclear. Events that are unique and not similar to EAS are the subject of the study presented in this paper. Events such as gamma-ray bursts (GRBs), out-of-aperture upward going EASs accompanied by lightning flashes, as well as terrestrial gamma-ray flashes (TGFs) are considered as their possible sources.

The High-Energy Ray Observatory (HERO) is a space experiment based on a heavy ionization calorimeter for direct study of cosmic rays. The effective geometrical factor of the apparatus varies from 12 to 60 m$^2$sr for protons depending on the weight of the calorimeter from 10 to 70 tons. During the exposure for $\sim$5 years this mission will make it possible to measure energy spectra of all abundant cosmic ray nuclei in the knee region ($\sim$3 PeV) with individual resolution of charges with energy resolution better than 30\% and provide useful information to solve the puzzle of the cosmic ray knee origin. HERO mission will make it also possible to measure energy spectra of cosmic rays nuclei for energies 1-1000 TeV with very high precision and energy resolution (up to 3\% for calorimeter 70 tons) and study the fine structure of the spectra. The planned experiment launch is no earlier than 2029.

The orbital detector TUS (Tracking Ultraviolet Setup) with high sensitivity in near-visible ultraviolet (tens of photons per time sample of 0.8 μ s of wavelengths 300–400 nm from a detector’s pixel field of view) and the microsecond-scale temporal resolution was developed by the Lomonosov-UHECR/TLE collaboration and launched into orbit on 28 April 2016. A variety of different phenomena were studied by measuring ultraviolet signals from the atmosphere: extensive air showers from ultra-high-energy cosmic rays, lightning discharges, transient atmospheric events, aurora ovals, and meteors. These events are different in their origin and in their duration and luminosity. The TUS detector had a capability to conduct measurements with different temporal resolutions (0.8 μ s, 25.6 μ s, 0.4 ms, and 6.6 ms) but the same spatial resolution of 5 km. Results of the TUS detector measurements of various atmospheric emissions are discussed and compared to data from previous experiments.

The NUCLEON satellite experiment is designed for direct measurements of the energy spectra of cosmic-ray nuclei and the chemical composition (Z=1−30) at an energy range up to 1000 TeV. The energy spectra of protons and helium nuclei are presented. Some spectral peculiarities were found. The differences of protons and helium spectra are investigated.

The physics motivations and characteristics of the new gamma-experiment TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) are presented. The TAIGA experiment addresses ground-based gamma-ray astronomy at energies from a few TeV to several PeV, as well as cosmic ray physics from $100$ TeV to several EeV. For the energy range $30 - 200$ TeV the sensitivity of the planned for future extension of TAIGA up to $5$ km$^2$ area for detection of the local sources is expected to be $10^{-13}$ erg cm$^{-2}$ sec$^{-1}$ for $500$ h of observation. The combination of the wide angle Cherenkov timing detectors of the TAIGA-HiSCORE array and the $4$ m class Imaging Atmospheric Cherenkov Telescopes of the TAIGA-IACT array with their FoV of $10x10$ degrees offers a cost effective-way to construct a $5$ km$^2$ array. Reconstruction of an EAS energy, direction and core position based on the TAIGA-HiSCORE data will allow us to increase the distance between comparatively expensive IACTs up to $800 - 1200$ m. The low investments together with the high sensitivity for energies $\geqslant 30-50$ TeV make this pioneering technique very attractive for exploring the galactic PeVatrons and cosmic rays. In addition to the Cherenkov light detectors we intend to deploy an array of muon detectors (TAIGA-Muon array) over an area of 1 km$^2$ with a total area of about $2000 - 3000$ m$^2$. The TAIGA-IACT-HiSCORE together with the TAIGA-Muon array will be used for selection of gamma-ray induced EAS. At present the first stage of TAIGA have been constructed in the Tunka valley, $\sim 50$ km West from the Lake Baikal in Siberia. Now it consists of 28 TAIGA-HiSCORE Cherenkov stations distributed over an area of $0.25$ km$^2$ and the first IACT of the TAIGA-IACT array. We are planning to test operation of the single telescope in coincidence with the HiSCORE up to shower impact distances of $\sim 500 - 600$ m; for this purpose we already started construction of the second imaging telescope at $300$ m distance from the first one. During 2017 -- 2019 years we intend to increase the number of the TAIGA-HiSCORE stations up to $100 - 120$, spread on the area of $1$ km$^2$ and to deploy $2$ additional IACTs.

The orbital NUCLEON detector was launched at 26 December 2014 for 5 years of data taken.The experiment is designed to measure cosmic ray energy spectrum and charge composition at 100 GeV -1000 TeV and Z = 1-30 respectively.The NUCLEON apparatus structure, methods of primary cosmic ray charge and energy measurements are described.Preliminary results of the measurements of the cosmic nuclei energy spectra and the charge composition are presented from the first year and a half of data taking from orbit.

The "Lomonosov" satellite, with the TUS instrument on board, was launched on April 28, 2016 on solar-synchronized orbit with altitude about 500 km. The main goal of the TUS space experiment is to search the Ultra High Energy Cosmic Rays (UHECR) at E >~70 EeV by measuring the fluorescence and Cherenkov radiation of extensive air showers (EAS) in the Earth's atmosphere. The TUS instrument's design and principles of operation are briefly presented. A multi-level algorithm for the search of EAS-like events was developed and applied to the TUS data set analysis. The preliminary results of the off-line reconstruction program for data analysis, search and study of candidates for the UHECR event are described and its parameters as statistical characteristics and arrival directions are presented.

The TUS space experiment is aimed to study the energy spectrum and arrival direction of Ultra High Energy Cosmic Rays (UHECR) at E ~ 1020 eV by measuring the fluorescence yield of EAS in the atmosphere. The "Lomonosov" satellite, with TUS, was launched at the April 16, 2016. Satellite now is in orbit and fully operational. The TUS collaboration plans to design and produce a ground-based system of light sources for the in-flight calibration of the TUS detector. Two types of the possible UV light sources are presently under consideration for this purpose: LEDs and laser stations. The design and fabrication of the TUS ground-based calibration light source prototypes based on LedEngin-LZ4-00U600 LEDs and on the use of the "Simeiz-1873" laser stations are presented.

The TUS space project for investigation of Ultra High Energy Cosmic Rays (UHECR) by the measurement of Extensive Atmospheric Shower fluorescent radiation is in the construction stage. The main goal of the TUS mission is to search for cosmic ray particles beyond the GZK energy limit. The observation of the full sky for primary particle arrival directions is an advantage of the TUS project in comparison to the ground based experiments. The TUS experience of UHECR study from the space will be of importance for future space detectors like the JEM-EUSO mission. The TUS detector operation could be considered as a ”pathfinder” for the JEM-EUSO mission including the JEM-EUSO UV sensor test. The technological TUS prototype is produced and their tests are in progress. The flight detector has to be produced in 2010-2011. The mission is planned for operation at the end of 2011 at the dedicated “Mikhail Lomonosov” satellite.

The FLUKA code is used to check the method (proposed earlier for the INCA project) of detection of MeV-range neutrons originated in nuclear and pure electromagnetic cascades in multilayer image lead-scintillator calorimeter (with an admixture of cadmium or gadolinium) without neutron counters by delayed ionization. MeV-range neutrons lose their energy during several microseconds in collisions with light nuclei, diffuse, and become captured by Cd or Gd nuclei with subsequent emission of gamma-rays which, in their turn, are converted into electrons. Amplitudes, time windows, a lateral spreading of delayed ionization produced by these electrons in scintillator layers are calculated. It is shown that neutron signal measured by this way can be highly efficient for the separation of electron-initiated cascades from the proton-initiated ones up to energies of several TeV. This method is planned to be used in the new space projects HERO (High Energy cosmic Ray Observatory) and INCA (Ionization-Neutron Calorimeter) aimed at investigation of different species of high-energy cosmic radiation (protons, nuclei, electrons, diffuse gammaray emission) with a high accuracy.