1. JINR astrophysical studies JINR astrophysical studies in the NUCLEON and TUS space experiments Alushta-2013. Tkachev

2. Galactic: supernova remnants? extragalactic: gamma ray bursts? ТUS NUCLEON Alushta-2013 L. Tkachev

3. NUCLEON experiment status Alushta-2013 L. Tkachev SINP MSU, Moscow “Gorizont”, Ekaterinburg НИИ Материаловедения, Zelenograd JINR, Dubna Frunze Arsenal Design Bureau, St.-Petersburg

4. Knee Прямые измерения There is a large difference in data for the CR nuclear component flux and composition around of the knee region Alushta-2013 L. Tkachev

5. Эксперимент АМS-2 Эксперимент АМS-2

8. Galactic cosmic ray anisotropy Alushta-2013 L. Tkachev

9. The arrival direction of cosmic-ray muons recorded with 40 IceCube strings (Southern Hemisphere). The variations are of order 10 −3 on a uniform distribution. The color scale represents the relative intensity. The dots indicate the directions of Vela and Geminga - the brightest gamma-ray sources in the sky. Also shown is the muon data of Milagro obtained by the same method (Northern Hemisphere). Muon energy ≈ 20 ТэВ. The anisotropy contradicts to the average value of the galactic magnetic fields about of few μG: charge particle giroradius is ~0.1 pc for E ~ 100 TeV, distance up to Vela ~ 100 pc that is possible source of GCR. NUCLEON provides good statistics to study anisotropy. Medium scale anisotropy IceCube Milagro NUCLEON Alushta-2013 L. Tkachev

10. NUCLEON apparatus consists of - NUCLEON detector as a monoblock inside of pressure container, - Special telemetry system inside of separate container, - Antenna-fider system, - Mechanical support interface of the connection with base satellite system. Main NUCLEON parameters: -Total weight ~ 350 kg (for detector ~250 kg); - Power cunsumtion~150 W (for detectors ~ 120 W); - Telemetry ~270 MB/day; - Data taking period ≥5 years. Alushta-2013 L. Tkachev

11. NUCLEON detector + microcalorimeter Alushta-2011 L. Tkachev

12. The NUCLEON apparatus in assemble before combine tests

13. Beam tests at SPS CERN – 2011-2013 Dubna-2013 L. Tkachev

15. NUCLEON charge measuring test at 2013 CERN New NUCLEON cip test at 2013 CERN

16. Proton spectrum to be expected in the NUCLEON experiment (green crosshatched region) NUCLEON 3 year data taking Alushta-2013 L. Tkachev

17. Conclusion - NUCLEON  The flight NUCLEON copy was produced, tested at SPS CERN in 2011-2013 and is ready for assembling at the RESURS P №2 satellite.  The NUCLEON mission is planned for operation since the 2014 for 3 -5 years of data taking  Next step is HERO experiment. Alushta-2013 L. Tkachev

18. Ultra High Energy Cosmic Rays TUS experiment status Е > 4*10 19 эВ Alushta-2013 L. Tkachev - Skobeltsyn Institute of Nuclear Physics, MSU, Moscow, Russia - Joint Institute for Nuclear Research - Space Regatta Consortium, Korolev, Moscow region, Russia - Physics Department, EWHA Woman University, Seoul, Korea - University of Puebla, Puebla, Puebla, Mexico - University of Michiocan, Morelia, Michiocan, Mexico

19. The fluorescence EAS radiation may be measured by the ground or space detectors to get the longitudinal shower profile and obtain the UHECR parameters: energy, arrival direction and nature (proton or nuclear). A Cerenkov radiation reflected from the Earth surface or clouds may be measured from space also. Atmospheric conditions are much more stable in upper layers of the atmosphere that is important to reduce systematic uncertainty of the UHECR energy measurement. Alushta-2013 L. Tkachev

21. CRISIS 2009: MASS COMPOSITION Alushta-2013 L. Tkachev HiRES Auger

29. The main problems in UHECR: mass composition at 1 × 10 18 − 1 × 10 20 eV. origin of cutoff at E ~ 5 × 10 19 eV (GZK cutoff ?) DETECTION OF UHE GZK NEUTRINOS. search for the UHECR sources. theory of acceleration to the highest energies. Alushta-2013 L. Tkachev

30. The TUS is the main detector at the “Mikhail Lomonosov” satellite Alushta-2011 L. TkachevDubna-2013 L. Tkachev TUS will measure the EAS fluorescent radiation

31. JINR responsibility: Fresnel mirror production, tests and optical parameter measurements Alushta-2013 L. Tkachev

32. The TUS Fresnel mirror. Alushta-2013 L. Tkachev

33. Left: The Point Spred Function (PSF) angular dependence of the ideal TUS Fresnel mirror Right: The PSF angular dependence of the real TUS Fresnel mirror. The optical parameters measurement

34. TUS test at the ISTRA space center

35. TUS calibration in flight The UV light source on the drone or plane is the only possibility

37. Conclusion - TUS  The TUS mirrors were produced and tested in 2010-2012. It confirms reliability of the mirror design: carbon plastic and aluminum honeycomb.  The optical parameters of the mirror are measured and are in reasonable correspondence as with the Field-of-View of the TUS photo receiver as with PMT pixel size  The flight TUS model is ready for integration at the Mikhail Lomonosov satellite..  The TUS mission is planned for operation in 2014 for 3 years of data taking  TUS is the pilot experiment to confirm a possibility UHECR study from space. Next step is KLYPVE experiment on ISS. Alushta-2013 L. Tkachev