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From Cosmic Ray Physics to Gamma Astronomy In The TAIGA experiment: from cosmic ray physics to gamma-ray astronomy in the Tunka valley N.Budnev, Irkutsk State University For the TAIGA collaboration Gamma-astronomy & neutrino astronomy To understand a nature of an cosmic high energy accelerator one can detect gamma-rays or neutrinos. RX J1713.7 – remnant of a super- nova ..but relatively simple to detect .. but very difficult to detect At energy > 30 TeV An 1км3 neutrino detector - 1 event / 10 year An 1км2 gamma detector - 1 event / 3 hours! About 162 TeV energy gamma-ray sources were discovered . But only a few gamma- quantum with energy more then 50 TeV were detected up to now. An array with aria more then 1 sq. is required IACT - Imaging Atmospheric Cherenkov Telescopes About 200 sources of HEGRA gamma rays with energy HESS more than 1 TeV were discovered with IACT MAGIC arrays. VERITAS But no gamma- quantum S ~ 0.01 km2 with energy more then 80 TeV were detected up to Future Project now. An area of an array CTA should be 1 km2 at least! An IAST is narrow-angle camera Telescope (3-5 FOV) consisting of a mirror of 4 -24 m diameter which reflects EAS Cherenkov light into a camera where EAS image is formed Mirror with Diameter 4-24 m CTA project: 100 IACT on aria 7 кm2 An IACT-array must have >10000 channels / km2. Cost of the IACT array more than 100 millons $/ km2 Crab with HAWC (0.0225 km2) • The Crab is the brightest g source detected by HAWC and is used to refine the analysis, validate the simulations, and probe the highest energy emission g 60 TeV g-ray from the Crab Earth atmospheric shower detection with the Cherenkov wide angle timing arrays in the Tunka - Experiment EAS Cherenkov light EAS Energy g detection technique E = A · [Nph(200m)] g = 0.94±0.01 θ, φ Average CR mass A Xmax LnA ~ Xmax Xmax = C –D· lg τ (400) (τ(400) - width of a Cherenkov pulse at distance 400 m EAS core from) Xmax = F(P) X0 P -Steepness of a Lateral Distribution Function (LDF) Tunka-133 array:175 Cherenkov detectors distributed on 3 km2 area (2006-2012y) 1 км 50 km from Lake Baikal Tunka Collaboration N.M. Budnev, O.A. Chvalaev, O.A. Gress, A.V.Dyachok, E.N.Konstantinov, A.V.Korobchebko, R.R. Mirgazov, L.V. Pan’kov, A.L.Pahorukov, Yu.A. Semeney, A.V. Zagorodnikov Institute of Applied Phys. of Irkutsk State University, Irkutsk, Russia; S.F.Beregnev, S.N.Epimakhov, N.N. Kalmykov, N.I.KarpovE.E. Korosteleva, V.A. Kozhin, L.A. Kuzmichev, M.I. Panasyuk, E.G.Popova, V.V. Prosin, A.A. Silaev, A.A. Silaev(ju), A.V. Skurikhin, L.G.Sveshnikova I.V. Yashin, Skobeltsyn Institute of Nucl. Phys. of Moscow State University, Moscow, Russia; B.K. Lubsandorzhiev, B.A. Shaibonov(ju) , N.B. Lubsandorzhiev Institute for Nucl. Res. of Russian Academy of Sciences, Moscow, Russia; V.S. Ptuskin IZMIRAN, Troitsk, Moscow Region, Russia; Ch. Spiering DESY-Zeuthen, Zeuthen, Germany; A.Chiavassa Dip. di Fisica Generale Universita' di Torino and INFN, Torino, Italy. Advantage of the Tunka-133 array: 1. Good accuracy positioning of EAS core (5 -10 m) 2. Good energy resolution (~ 15%, in principal up to - 5% ) 2. Good accuracy of primary particle mass identification 2 (accuracy of Xmax measurement ~ 20 -25 g/cm ). 3. Good angular resolution (~ 0.5 degree) 4. Low cost: the Tunka-133 – 3 km2 array ~ 106 Euro Disadvantage: Short time of operation ( moonless, cloudless nights) – 5-10% An event example Hitted detectors A ADF ADF Amplitude distant function & LDF LDF Lateral Distribution function Delay time vs. Distance from core T ns = (R+200/R0 )2 ×3.3 ns WDF – width distant function The all particles energy spectrum I(E)·E3 energy resolution ~ 15%, in principal up to - 5% -Tunka-25 --Tunka-133 First knee . Second knee 1. Agreement with KASCADE-Grande, Ice-TOP and TALE (TA Cherenkov). 2. The high energy tail do not contradict to the Fly’s Eye, HiRes and TA spectra.. Mean Depth of EAS maximum Mean logarithm of primary mass. -2 Xmax g·cm The primary CR mass composition changes from light (He) to heavy up to energy ~ 30 PeV A lightening of the mass composition take place for starting from an energy 100 PeV From Tunka Collaboration to TAIGA Collaboration Irkutsk State University (ISU), Irkutsk, Russia Scobeltsyn Institute of Nuclear Physics of Moscow State University (SINP MSU), Moscow, Russia Institute for Nuclear Research of Russian Academy of Science (INR RAN), Moscow, Russia Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation of RAS (IZMIRAN), Troitsk, Russia Joint Institute of Nuclear Physics (JIRN), Dubna, Russia National Research Nuclear University (METHI), Moscow, Russia Budker Institute of Nuclear Physics SB RAS (BINP), Novosibirsk, Russia Novosibirsk State University (NSU), Novosibirsk, Russia Deutsches Elektronen Synchrotron (DESY), Zeuthen, Germany Institut für Kernphysik, Karlsruhe Institute of Technology (KIT), Karlsruhe, Germany Institut fur Experimentalphysik, University of Hamburg (UH), Germany Max-Planck-Institut für Physik (MPI), Munich, Germany Fisica Generale Universita di Torino and INFN, Torino, Italy ISS , Buharest, Rumania Towards Very High Energy Gamma-Ray Astronomy array at Tunka Valley TAIGA – Tunka Advanced Instrument for cosmic rays and Gamma Astronomy – 5 arrays = + Tunka-133 Tunka-Rex + + + TAIGA-Muon (including TAIGA-HiSCORE array -net of TAIGA-IACT array -net of non imaging 500 wide-angle 16 Imaging Atmospheric Tunka – Grande) array net stations distributed on area 5 km2 Cherenkov Telescopes with of scintillation detectors, Angular resolution – 0.1 deg, mirrors – 4.2 m diameter. including underground Core position - 5-10 m muon detectors with area - 2 3 2 Energy resolution 10 – 15% Charged particle rejection 10 2 10 m area using imaging technique. Pulse form - hadron rejection. Charged particle rejection. Gamma-ray Astronomy Main Topics Search for the PeVatrons. for the TAIGA VHE spectra of known sources: where do they stop? observatory Absorption in IRF and CMB. Diffuse emission: Galactic plane, Local supercluster. Charged cosmic ray physics Energy spectrum and mass composition anisotropies from 1014 to1018 eV. 108 events (in 1 km2 array) with energy > 1014 eV TAIGA Particle physics energy range Axion/photon conversion. For γ and CR Hidden photon/photon oscillations. Lorentz invariance violation. pp cross-section measurement. Quark-gluon plasma. Point source sensitivity of TAIGA to gamma rays TAIGA: Imaging + non-imaging techniques Muon detectors TAIGA - HiSCORE: core position, direction and energy reconstraction. Gamma/ hadron separation : TAIGA-IACT - (image form, monoscopic operation) & TAIGA-Muon (electron/muon ratio) Q-factor for common operation of TAIGA-IACT & TAIGA-HiSCORE - fraction of gamma ray Events - background events After selection TAIGA-HiSCORE (High Sensitivity Cosmic Origin Explorer) • Wide-angle time- amplitude sampling non-imaging air Cherenkov array. 700 detectors on area 5 km2 • Spacing between Cherenkov stations 80-100 m ~ 100 -150 channels / km2. Accuracy positioning EAS core - 5 -6 m Angular resolution : ~ 0.1-0.3 degree Energy resolution ~ 10 - 15% Accuracy for Xmax 20 -25 g/cm2 DRS-4 board ( 0.5 ns step) TAIGA-HiSCORE 2017 year setup 60 detectors on area (S=0.6 km2 ) TAIGA-HiSCORE (0.25 км2) results (PRELIMINARY!) E< 100 TeV Excess > σ) RA = 83.63° DEC = 22°.00” Very preliminary TAIGA-HiSCORE Search for the Crab Energy spectrum with TAIGA-HiSCORE The TAIGA – IACT array The TAIGA- IACT array will include 16 Imaging Atmospheric Cherenkov Telescopes distributed with 600 – 1000 m spacing over an area of 5 km2. Each HEGRA-like telescope of the array will be composed of a mosaic, 34-segment reflector in Davis-Cotton design, with a diameter of individual mirrors 60 cm. The full diameter of the reflector is 4.3 m, the area ~10 m2, the focal length 4.75 m. The TAIGA- IACT operate together with Tunka-133, Tunka-Rex, TAIGA-HiSCORE and TAIGA-Muon . Threshold energy ~ 1 TeV The sensitivity in the energy range 1-20 TeV is 10-12 erg cm-2 s-1 (for 50 hours of observation) The sensitivity in the energy range 30-200 TeV -13 -2 -1 is 10 erg cm s (for 10 events in 500 hours of observation) Low cost – 400 000$ / unit Assembling of the 1st mount. Conceptual design of the TAIGA IACT camera mechanics Outside case Camera opening lid Ventil for volume ventilation MAROC-3 based Trigger, DAQ & Slow Control System Power supplies, could be set outside camera, in a separate box PMT-modules Connections Plexiglas window, sealed system Light guides PCB HV system T° and pressure control, forced ventilation system 27 The Camera of the TAIGA-IACT Camera : 547 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 9.6х9.6 deg Basic cluster: 28 PMT-pixels. Signal processing: PMT DAQ board based on the MAROC3 ASIC Inside of the camera The mirrors alignment (HEGRA approach) 800 m A light source at 800 m from the telescope Mirror Screen A diameter of a spot of reflected light – 5 mm Integral SIZE-spectrum 2102 Experiment 102 All pixel Nphel>0 Npix>6, size>50,Cl: 12,6 101 Npixels>6 Joint events with Hiscore Npix>6,size>50 Cl:12,6 1 - All events 0 -1 10 Calculation new 3-1000 TeV 10-1 100-1000 TeV -2 N(>size)/t, sec 10 E =700 TeV N(>size) sec 200 m from IACT Joint events 10-3 (IACT + HiSCORE) 10-4 101 102 103 104 105 size, ph.el. SIZE, P..E Size(IACT)& Size (HiSCORE) Qtel_PhEl=QtelChp*17400cm2*0.1*0.3 (Qef=0.1,ef=0.3) All events 200217 Events s S<0.02 o o 104 .0 < Bet<3 Rc<20 cm size 3 Size(IACT) 10 102 102 103 104 105 SIZEQtel_Pel_exp (from HiSCORE Data) Tunka-Rex (Tunka –Radio Extention) array 63 antenna stations triggered by Tunka-133, Tunka-Grande and TAIGA-HiSCORE arrays - Common operation with Tunka- 133, TAIGA-HiSCORE and Tunka- Grande scintillation array - Cross calibration of Radio and Cherenkov methods - Radio reconstruction precision - Crucial input to next generation The gain G over zenith angle at 50MHz of the cosmic-ray observatories SALLA for dierent ground conditions.
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