Participating Countries and International Organizations:
Czech Republic, Germany, Japan, Italy, Mexico, Republic of Korea, Romania, Russia, Ukraine. 
Scientific Programme:

• The main topic of multi-messenger TAIGA array are Gamma-ray astronomy, charged cosmic ray physics\\ and particle physics. Gamma-ray astronomy - one of the most intriguing questions in high-energy astropar-\\ticle physics is a search for galactic objects for accelerating of particles up to PeV-energies (thr so-called Pevatrons); VHE spectra of known sources: where do they stop; absorption in IR and CMB; diffuse emission from galactic plane and local supercluster.Charged cosmic ray physics - the energy spectrum and mass composition measurements from 10 ¹⁴ to 10 ¹⁸ eV. Particle physics - axion/photon conversion; hidden photon/photon oscillations; Lorentz invariance violation; pp cross-section measurement; search for quark-gluon plasma phenomena. 
  
  
• The TUS space experiment has been proposed to measure the energy spectrum, composition and angular distribution of the Ultra High Energy Cosmic Rays (UHECR) at E  10 ¹⁹-10 ²⁰ eV, to study the region beyond the GZK cutoff. Existence of these particles is beyond the Standard Model of particle physics and is of great interest. The study from the orbit is much more effective in comparison with the ground-based detectors. The existing world statistics is assumed to be increased by a factor of 2 during 3 years of the global data taking. The TUS detector will make it possible to study UHECP neutrino Extensive Air Showers (EAS) from the space orbit. 
  
  
• The aim of the NUCLEON Project is direct CR measurements in the energy range 10 ¹¹-10 ¹⁵ eV and the atomic charge range up to Z30 in the near-Earth space to solve mainly the "knee" problem in the CR spectrum. The CR phenomena in this energy region are investigated in terrestrial experiments by measurement of EAS parameters or in balloon or space experiments. Below ~ 10 ¹⁴ eV the spectrum and composition are known from direct observation with detectors placed in balloons and earth satellites. However, at higher energies the CR flux is smaller and more difficult for direct and needs observation. Precise measurement of the CR composition and anisotropy will help to test the existing theoretical concepts and will become a basis for further studies.

Expected main results in 2018:

• Design and production of second IACT for TAIGA experiment. 
  
  
• Participation in the MC simulation of TAIGA experiment and data analysis. 
  
  
• The calibration TUS detector on the Earth orbit. 
  
  
• Participation in the data taking of the TUS experiment and data analysis. 
  
  
• Participation in the data taking of the NUCLEON experiment and data analysis.