The TAIGA experiment - a hybrid detector for very high energy gamma-ray astronomy and cosmic ray physics in the Tunka valley

Transcription

1 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

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

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

4 Non-Imaging Timing array Тunka-133: 175 wide angle Cherenkov detectors over 3 km 2 ( ) 1 km The all particle energy spectrum I(E) E 3

5 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

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

7 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. TAIGA energy range For γ and CR Charged cosmic ray physics Energy spectrum and mass composition anisotropies from to10 18 ev events (in 1 km 2 array) with energy > ev Particle physics Axion/photon conversion. Lorentz invariance violation. pp cross-section measurement. Quark-gluon plasma.

8 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 Cherenkov detectors of the Tunka-133 array 350 h of good weather operation (October-February, 2017) events ( 4 stations) Angular resolution ~ deg

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

10 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

11 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

12 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.

13 The Camera of the TAIGA-IACT 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

14 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

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

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

17 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

18 Upgrades of the TAIGA experiment Funded TAIGA upgrade : - 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 IACTs

19 TAIGA Status 2016 TAIGA-HiSCORE TAIGA-IACT

20 TAIGA Status 2019 TAIGA-HiSCORE 109 detectors 3 TAIGA-IACT 1km IACT

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

22 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 ±15% variation (minimum to maximum). A clear peak in amplitude spectrum is seen from cosmic muons in a self trigger mode. ¼ of full scale detector PMT

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

24 TAIGA Integral point source sensitivity

25 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: TeV/cm 2 /s (300 hr TeV) Future option: - 5 km 2 array: 500 wide-angle stations IACTs - point source sensitivity: ~10-13 TeV/cm 2 /s