The TAIGA experiment - a hybrid detector for very high energy - PowerPoint PPT Presentation

The TAIGA experiment - a hybrid detector for very high energy gamma-ray astronomy and cosmic ray physics in the Tunka valley N. Budnev, Irkutsk State University For the TAIGA collaboration

The TAIGA experiment - a hybrid detector for very high energy gamma-ray astronomy and cosmic ray physics in the Tunka valley TAIGA – T unka A dvanced I nstrument for Cosmic Ray and G amma A stronomy N. Budnev, Irkutsk State University For the TAIGA collaboration

Two ways of EAS Cherenkov light detection in gamma-astronomy and cosmic ray physics Non-imaging timing Cherenkov Imaging Cherenkov arrays - HEGRA, HESS, MAGIC, VERITAS… arrays - Tunka valley. S ~1 km 2 Atmosphere as a huge calorimeter S ~0.01 km 2

Non-Imaging Timing array Т unka-133: 175 wide – angle Cherenkov detectors over 3 km 2 (2009....2012…) The all particle energy spectrum I(E)·E 3 1 km

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 RAS (INR), 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 (MEPhI), 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 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 , Bucharest, Rumania

TAIGA: combine Imaging + Non-Imaging technique IACT IACT IACT IACT IACT Hybrid concept IACT operated in Mono-Mode at large distances IACT IACT HiSCORE (Timing): direction, core location, energy IACT (Imaging): gamma – hadron separation

Energy range and main topics for the TAIGA experiment Gamma-ray Astronomy Search for the PeVatrons. VHE spectra of known sources: what are the highest energy? Absorption in IRF and CMB. Diffuse emission: Galactic plane, Local supercluster. Charged cosmic ray physics Energy spectrum and mass composition anisotropies from 10 14 to10 18 eV. 10 8 events (in 1 km 2 array) TAIGA with energy > 10 14 eV energy range For γ and CR Particle physics Axion/photon conversion. Lorentz invariance violation. pp cross-section measurement. Quark-gluon plasma .

TAIGA-HiSCORE : Array of Timing stations (2016: 0.25 km 2 ) HiSCORE = High Sensitivity Cosmic Ray Origin Explorer Stations with large FOV: ~ 0.6 sr Spacing: 106 m 350 h of good weather operation (October-February, 2017). 2 10 7 events ( ≥ 4 stations) Cherenkov detectors Angular resolution ~ 0.1 – 0.3 deg of the Tunka-133 array

First TAIGA-HiSCORE results (0.25 км 2 ) A hint of signal compatible with expectation (~40 TeV < E< 100 TeV) RA = 83.63 ° DEC = 22 °.00” Very preliminary Energy spectrum Tentative Crab-search

First TAIGA-HiSCORE results (0.25 км 2 ) CATS Lidar, 532 nm, 4 khz, 10^13y/m2 • Excellent HiSCORE calibration source – flat timing profile - precision pointing Precision verification with Laser on-board International Space Station (ISS) <0.1deg

TAIGA-HiSCORE Other presentation on the conference: 1. M.Tluczykont et al TAIGA-HiSCORE: results from the first two operation seasons 2. L.Sveshnikova et al. Search for gamma-ray emission above 50 TeV from Crab Nebula with the TAIGA detector 3. R.Wischnewski et al TAIGA-HiSCORE observation of the CATS-LIDAR on the ISS as fast moving point source

The TAIGA – IACT The first TAIGA - IACT Is in commissioning since early 2017 : - 34-segment reflectors (Davis-Cotton) - Diameter 4.3 m, area ~10 m 2 - Focal length 4.75 m - Threshold energy ~ 1.5 TeV Next 2 IACTs in construction. The final IACT array will include 16 IACTs over 5 km² with > 600 m spacing (i.e. in “mono - mode”). Will be operated in Hybrid-Mode, with TAIGA-HiSCORE, TAIGA-Muon.

The Camera of the TAIGA-IACT - 547 PMTs ( XP 1911) with - 15 mm useful diameter of photocathode - Winston cone: 30mm input size - each pixel = 0.36 deg - FOV 10 x 10 deg Basic cluster: 28 PMT-pixels. Signal processing: PMT DAQ board based on MAROC3 ASIC

TAIGA-IACT and TAIGA-HiSCORE : Images of common events Red lines show the directions to the EAS core position, reconstructed by using the TAIGA-HiSCORE array data. Black lines show the major axes as obtained from the IACT images

TAIGA-IACT: Integral Size-spectrum E =700 TeV 200 m from IACT Experiment: all detected events - red line ( size = sum of p.e. common events - black line. in the image ) Monte Carlo predictions: 3 – 1000 TeV - red circles 100 – 1000 TeV - black circles.

Size (IACT) vs. Size (HiSCORE) February, 2017 1 st TAIGA- IACT threshold – 20 Tev (6 mirrors) TAIGA-IACT Counting rate - 1 Hz Common event - 0.3 Hz (all detected by TAIGA-HiSCORE events in TAGA-IACT view).

TAIGA-IACT: design and first results Other presentation on the conference: 1. N. Lubsandorzhiev et al (TAIGA Collaboration) Camera of the first TAIGA-IACT: construction and calibration 2. L. Sveshnikova et al (TAIGA Collaboration) Commissioning the joint operation of the wide angle timing HiSCORE Cherenkov array with the first IACT of the TAIGA experiment 3. D. Zhurov et al (TAIGA Collaboration) Software design for the TAIGA-IACT telescope pointing and control system

Upgrades of the TAIGA experiment Funded TAIGA upgrade 2017-2019: - HiSCORE 0.25 km 2 (2016)  1 km 2 (2019) - two more IACTs - Muon detectors (200m 2 ) Long term plan: Upgrade up to 5km 2 array + 10-16 IACTs

TAIGA Status 2016 TAIGA-HiSCORE TAIGA-IACT

TAIGA Status 2019 TAIGA-HiSCORE 109 detectors 1km 2 + 3 IACT 3 TAIGA-IACT

Maximizing the TAIGA-HiSCORE Sensitivity: Remote station inclination adjustment during operation Crab, 220 hours Tycho, 290 hours, Tilting on 25 ° to South Vertica l per year per year

The TAIGA-Muon particle counter. :  Counter dimension 1x1 m 2.  Wavelength shifting bars are used for collection of the scintillation light on the PMT  Mean amplitude from cosmic muon is 23.1 photoelectrons with ¼ of full scale detector ± 15% variation (minimum to 25.9 22.9 21.8 26.1 22.6 maximum).  A clear peak in amplitude 24.4 20.4 21.2 spectrum is seen from cosmic 22.2 muons in a self trigger mode . PMT

TAIGA: A possible future 5km 2 upgrade TAIGA – Tunka Advanced Instrument for cosmic rays and Gamma Astronomy + + TAIGA-Muon (including TAIGA-HiSCORE - array Tunka – Grande) - array of of 500 non imaging wide- scintillation detectors, TAIGA-IACT - array -of 10 - angle detectors distributed including underground 16 IACT with mirrors – 4.2 on area 5 km 2 . muon detectors with area - m diameter. An EAS core position, 10 2 2 10 3 m 2 area Charged particles rejection direction and energy Charged particles rejection. using imaging technique . reconstruction.

TAIGA Integral point source sensitivity

Conclusions TAIGA aims at establishing a new, hybrid gamma-ray detection technology for >50 TeV TAIGA in 2016/17: 0.25 km 2 array + first IACT Commissioning seasons were successful - Stable operation, precision calibration in progress, E th ~50TeV - CR energy spectrum below the knee - Hint of a signal from Crab (in agreement with expectation) - Precision absolute pointing: from Laser on-board ISS - Joint operation of HiSCORE and IACT: first results TAIGA full scale prototype in 2019 (funding complete) - 1 km 2 array: 109 wide-angle stations + 3 IACTs - point source sensitivity: 2.5 10 -13 TeV/cm 2 /s (300 hr 30 – 200 TeV) Future option: - 5 km 2 array: 500 wide-angle stations + 10-16 IACTs - point source sensitivity: ~10 -13 TeV/cm 2 /s