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JINR astrophysical studies in the NUCLEON and TUS space experiments

JINR astrophysical studies in the NUCLEON and TUS space experiments. Alushta-201 3 . Tkachev. NUCLEON. Galactic: supernova remnants?. extragalactic: gamma ray bursts?. Т US. Alushta-201 3 L. Tkachev. NUCLEON experiment status. SINP MSU, Moscow “Gorizont”, Ekaterinburg

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JINR astrophysical studies in the NUCLEON and TUS space experiments

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

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

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

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

  5. Эксперимент АМS-2

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

  7. NUCLEON Medium scale anisotropy Milagro IceCube The arrival direction of cosmic-ray muonsrecorded with 40 IceCube strings (Southern Hemisphere).The variations are of order 10−3 on a uniformdistribution. The color scale represents the relativeintensity. The dots indicate the directions of Vela and Geminga - thebrightest gamma-ray sources in the sky.Also shown is the muon data of Milagro obtained by thesame 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. Alushta-2013 L. Tkachev

  8. NUCLEON apparatusconsists of - NUCLEON detector as a monoblock inside of pressure container, - Special telemetrysystem 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 ~250kg); • - Power cunsumtion~150 W (for detectors ~ 120 W); • - Telemetry ~270 MB/day; • - Data taking period ≥5years. Alushta-2013 L. Tkachev

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

  10. The NUCLEON apparatus in assemble before combine tests

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

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

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

  14. Conclusion - NUCLEON • The flight NUCLEON copywas produced, testedat SPS CERN in 2011-2013 and is ready for assembling at the RESURS P №2 satellite. • The NUCLEON mission isplanned for operation sincethe 2014 for 3 -5 years of data taking • Next step is HEROexperiment. Alushta-2013 L. Tkachev

  15. Ultra High Energy Cosmic RaysTUS experiment statusЕ > 4*1019 эВ - 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 Alushta-2013 L. Tkachev

  16. 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

  17. Alushta-2013 L. Tkachev

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

  19. The main problems in UHECR: • mass composition at 1 × 1018− 1 × 1020eV. • origin of cutoff at E ~5 × 1019eV (GZK cutoff ?) • DETECTION OF UHE GZK NEUTRINOS. • search for the UHECR sources. • theory of acceleration to the highest energies. Alushta-2013 L. Tkachev

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

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

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

  23. The optical parametersmeasurement Left: The Point Spred Function (PSF) angular dependence of the ideal TUSFresnel mirror Right: The PSF angular dependence of the real TUS Fresnel mirror.

  24. TUS testatthe ISTRA spacecenter

  25. TUS calibrationinflight The UV lightsourceonthedroneorplaneistheonlypossibility

  26. Conclusion - TUS • The TUS mirrors wereproducedandtested in 2010-2012. It confirms reliability of the mirror design: carbon plastic and aluminum honeycomb. • The optical parameters of the mirror aremeasuredandare in reasonable correspondence as with the Field-of-View of the TUS photo receiver as with PMT pixel size • The flight TUSmodelis ready for integration at the MikhailLomonosovsatellite. . • The TUS mission isplanned for operation in2014 for 3 years of data taking • TUS is the pilot experiment to confirm a possibility UHECR study from space. Next step is KLYPVEexperiment on ISS. Alushta-2013 L. Tkachev

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