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Участие ОИЯИ в проекте TAIGA

Участие ОИЯИ в проекте TAIGA. (Tunka Advanced Instrument for cosmic rays and Gamma Astronomy). Moscow State University, D.V.Skobeltsyn Institute of Nuclear Physics (Moscow) Joint Institute for Nuclear Research (Dubna) ИЗМИРАН (Moscow) DESY (Zeuthen) MPI for Physics (Munich),

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Участие ОИЯИ в проекте TAIGA

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  1. Участие ОИЯИ в проекте TAIGA (Tunka Advanced Instrument for cosmic rays and Gamma Astronomy) Moscow State University, D.V.Skobeltsyn Institute of Nuclear Physics (Moscow) Joint Institute for Nuclear Research (Dubna) ИЗМИРАН (Moscow) DESY (Zeuthen) MPI for Physics (Munich), Humboldt University (Berlin) Irkutsk State University (Irkutsk) University of Hamburg (Hamburg) Institute for Nuclear Research of RAS (Moscow) MEPhI (Moscow) Institute of Space Science , ISS (Bukarest) Karlsruhe Institute of Technology, KIT (Karlsruhe). This list does not agreee with that on page 4 !!

  2. JINR authors: V. Boreyko, N. Gorbunov, V. Grebenyuk, A. Grinyuk, A. Kalinin, M. Finger, Nguen Man Shat, S. Porokhovoy,V.Romanov, B. Sabirov,S. Slepnev, M. Slunecka, V. Sluneckova, A. Timoshenko, A. Tkachenko, L. Tkachev, N.Zaikova

  3. Towards a unique hybrid detector for gamma rays and cosmic rays at the high-energy end of galactic sources TAIGA – Tunka Advanced Instrument for cosmic rays and Gamma and Astronomy The concept: a hybrid array made of: Net of imaging detectors with mirrors , each 10 m2 square. Net of muon detectors 1022 103 m2 area. Net of non-imaging wide-angle optical stations (HiSCORE)

  4. TAIGA Collaboration Germany Russia Hamburg University (Hamburg) MSU/SINP (Moscow) DESY (Zeuthen) ISU (API) (Irkutsk) MPI for Physics (Munich) INR RAS (Moscow) Humboldt University(Berlin) JINR (Dubna) MEPHI (Moscow) IZMIRAN (Moscow) Italy Kurchatov Institute (Moscow) IPSM (Ulan-Ude) Torino University (Torino)

  5. Gamma-ray astronomy at > 30 TeV ~150 sources observed above 1 TeV < 10 sources observed above 30 TeV No photons detected above 100 TeV Where are the cosmic-ray Pevatrons ?

  6. Why data above 30 TeV are important It is generally believed that cosmic rays of energy at least to the knee ( 3·1015 ) are accelerated in our Galaxy SNRs ( Super Nova Remnants) are the favorite sites for the acceleration of of Galactic cosmic rays Gamma rays up to a few TeV have been observed from 7 SNRS

  7. But: The relative contribution of protons and electrons to the observed flux is still unclear Leptonic emission: inverse Compton scattering of electrons on low energy photos ( Cosmic Mircowave Background. Infrared, optical photons) Hadronic emission : π0 decay from proton interaction with thrr ambient nuclei In a few cases, the “hadronic footprint” has been probably observed, but proton energy doesn’t seem to reach the cosmic ray knee Gamma ray astronomy above 30 TeV could give the definitive answer of the question whether the SNRs are the long sought Pevatrons

  8. The main topics of the TAIGA array Multi –TeV gamma-ray astronomy - a search for galactic objects for accelerating of particles up to PeV-energies (the so-called Pevatrons); - VHE spectra of known sources: where do they stop; - diffuse emission from galactic plane and local supercluster. Charged cosmic ray physics - Study of the energy spectrum and mass composition measurements from 1014 to 1016eV at very high statistical level Particle physics - - axion/photon conversion; - hidden photon/photon oscillations; - Lorentz invariance violation; - pp and pA cross-section measurement; - search for quark-gluon plasma phenomena; - indirect search of dark matter particles

  9. Instruments Narrow angle of view – Imaging Air Cherenkov Telescopes (IACT) Wide angle (all sky) of view : Low energy threshold EAS arrays For effective suppression of the background it is important that the same EAS gives images in several telescopes (stereo approach). • Background suppression: • Excellent angular resolution • 2. Absence of muons

  10. Energy spectrum of gamma-rays: ~ E-2For multi-TeV gamma–ray astronomy we need an array withan area of more than 1 km2

  11. CTA ( Cherenkov Telescope Array) approach

  12. HiSCORE concept - Excellent angular resolution,- up to 0.1 degree - Energy threshold – up to 30 TeV . - Field of View (FOV) – 0.6 sr (±30 deq) - Low cost of each station – possibility to cover large area But: some problems with background suppression at low energies ! HiSCORE – Hundred* i Square-km Cosmic Origin Explorer

  13. TAIGA concept ~600 m Core position and direction of EAS by HiSCORe station, Background suppression by individual IACT (without needing stereo) The hybrid array of HiSCORE + Imaging detectors give superior background suppression !

  14. What we can see with 1 km2 array (short list)

  15. Status of array

  16. Tunka-133 array: 175 optical detectorson 3 km2 area 1 км Energy threshold - 1000 TeV

  17. Ways of threshold decreasing Eth ~ ( Sdet.η)-1/2(Tsignal )1/2 • Winston cones - PMT area increase in 4 times ( K = 1/ sin2 (tet) tet=30° - K =4 ) 2. Analog summation of signals in one station • Decreasing of Tsignal to7-10 ns 4. QE max = 35-40% 5.Using of wavelength shifter Winston cone

  18. 9 optical stations installed 36 PMT R5912 ( 8’’ ) DRS-4 board ( 0.5 ns step)

  19. Lateral Distribution (LDF) of Cherenkov light from gamma-ray induced EAS Egam = 30 TeV 1 Threshold flux 2 100 TeV Egam = 100 TeV 30 TeV 230 m 120 m

  20. HiSCORE 2014 32 stations – 0.3 km² array All stations are tilted on 25° tothe South 600 m 100 m spacing 450 m

  21. Threshold for gamma –ray flux 100 m spacing 150 m spacing

  22. Parameters of the Imaging Telescopes D = 4.32m F = 4.75m 34 mirrors with 60 cm diameters Camera : 400 PMTs ( XP 1911) with 15 mm useful diameter of photocathode Winston cone: 30 mm input size, 15 output size 1 single pixel = 0.36 deg full angular size 8.3 deg DAQ - MAROC3 First telescope to be commissioned (?) in autumn 2015

  23. CT3 of HEGRA CT3 of HEGRA

  24. Technical requirements for the IACT telescope • Spherical shape of the mirror facets of ~60 cm diameter with a total area of ~ 10 m2 • Turn range around horizontal axis (zenith angle) -10+95о, • Turn range around vertical axis (azimuthal angle) 0 - 360о. • Setting angular accuracy 0.01o. • Drive system – manual or remote-distance PC control with pecking motors • Rotation velocity – 1-2 degrees/sec. • The photo camera block of 750x750x400 mm2 size ~200 kg weight is fixed by carrier farms  FARMS or ARMS???????? at the focal 4000±1 mm distance from the mirror at the common with the mirror support structure • Operatiion conditions – temperature from minus 40 till plus 30o C - wind ~15 m/sec

  25. The first step for IACT construction: delivery of metal with camion

  26. Muon detectors Possibility to separate gamma-quanta induced showers is based on the fact that the number of muons in cosmic-ray induced showers is 30 times more than the number of muons in gamma-quanta induced showers. Because of the relatively low number of muons in EAS at such energies (the number of muons EAS from protons with energy of 100 TeV is 1000) the total area of muon detectors should be 0.2-0.3% of array total area and be 2000-3000 m2.

  27. Scintillation station from Kascade-Grande 19 stations 228 detectors ( 0.64 m2 ) on the surface 152 detectors undeground (muons detectors, total area 100 m2 Entrence to Muon detector

  28. Muon detector

  29. From 100 m2 to 2000 m2 muondetector area The price decreasing per unit of muon detector area is getting into the forefront.  WHAT DOES THAT MEAN? 1. Scintillation detectors of various types. 2. Water Cherenkov detectors on the basis of long (to 10 m) pipes. 3. Cherenkov detectors on the basis of water tanks of large area.

  30. Schedule of deployment 2014: 32 HiiCORE stations. 2015: Fist IACT and deployment of all 64 HiSCORE stations. Demonstration of scientific potential: measurement of energy spectrum of gammas from Crab Nebula 2016 : Deployment 4 IACTs. Starting deployment of muon detectors. Beginning of the physical program 2017-2018. Deployment of muon detectors

  31. Conclusion Participations in TAIGA experiment preparation - design and construction mechanics for Imaging Air Cherenkov Telescope (IACT) - production and test of IACT electronics Participations in TAIGA experiment simulation, data taking and data analysis

  32. Backup slides

  33. The technical requirements for the IACT telescope : • The spherical shape mirror facets of ~60 cm diameter and with a total mirror area of ~ 5 m2. • Focal distance ~4000±1 mm and FOV ~ ±5o. • Turn range around horizontal axis (zenith angle) -10+95о. • Turn range around vertical axis (azimuthal angle) 0-360о. • Setting angular accuracy 0.01o. • Drive system – manual and automatic. Remote-distance control with pecking motor by computer commands. Precise drive motors will be buying from a specialized company-producer. • Rotating velocity – 1 – 2 grad/sec. • The photo camera block of 750x750x400 mm2 size consists of 400 PMT matrix with FE and DAQ electronics. The PMT diameter will be 20-25 mm to provide the IACT angular resolution at the level of 0.02-0.03o. • The camera weight is ~200 kg and fixed by carrier farms at the focal 4000±1 mm distance from the mirror at the common with the mirror support structure. 10. Shift of the mutual mirror-camera position at the different IACT axis elevation is 1 – 2 mm. Service conditions – temperature from minus 40 till plus 30o C, wind up to 15 m/sec.

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