Status of the HiSCORE Project
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1 Status of the HiSCORE Project M. Tluczykont, D. Horns Tunka-HiSCORE, TAIGA HiSCORE Detector
2 Physics motivations & The HiSCORE concept Status of the 9-station Tunka-HiSCORE array Future plans: TAIGA and further prototyping
3 HiSCORE Hundred*i Square-km Cosmic ORigin Explorer Concept: non-imaging air Cherenkov technique Large area: up to few 100 km² Large Field of view: ~ 0.6 sr Sky-coverage: > π 200 h / year 2014: Astroparticle Physics, in press, 2014arXiv T 2013NIMPA H, arxiv: AdSpR T, astro-ph/ martin.tluczykont@physik.uni-hamburg.de
4 G Gamma-ray spectra Highest and morphology acceleration energies Diffuse Gamma-ray Diffuse emission Emission (Galaxy, local supercluster) E>10TeV s ay -r ic m os C am m ara ys Physics motivations Cosmic-ray spectroscopy Anisotropies Origin of cosmic Origin of rays cosmic rays Cosmic-ray Anisotropy Sub-knee pre-ankle Spectral fine-structure Nonstandard Propagation Propagation NucleonNucleon interaction Particle acceleration Dark matter Particle physics martin.tluczykont@physik.uni-hamburg.de E>100TeV
5 Cosmic rays HiSCORE Cosmic rays Adapted from Donato & Medina-Tanco 2008 Spectrum & composition in transition range Galactic / extragalactic origin martin.tluczykont@physik.uni-hamburg.de
6 Cosmic rays V Te Adapted from Donato & Medina-Tanco 2008 Gammas from Galactic Cosmic rays: Eγ ~ ECR/ martin.tluczykont@physik.uni-hamburg.de
7 Tevatron sky Gamma-rays > 100 GeV Hadronic? Leptonic?
8 Pevatron sky? Gamma-rays > 100 TeV
9 The Pevatron energy range? Gamma-rays
10 Accessing the pevatron sky very large area The HiSCORE concept
11 The HiSCORE concept Efficient instrumentation of very large areas: Picture: Serge Brunier Imaging air Cherenkov telescopes: O(1000) channels / km² Non-imaging air Cherenkov technique: O(100) channels / km² martin.tluczykont@physik.uni-hamburg.de
12 The HiSCORE concept Picture: Serge Brunier 0.5 m² station area: E thr Readout: GHz sampling Air shower m martin.tluczykont@physik.uni-hamburg.de 1ns time synch.
13 The HiSCORE concept Picture: Serge Brunier Air shower
14 The HiSCORE concept Picture: Serge Brunier Air shower
15 The HiSCORE concept Air shower
16 The HiSCORE concept
17 Physics potential of HiSCORE (gamma-ray astronomy)
18 Opening up the Pevatron range
19 Opening up the Pevatron range 100 km² / 1000h martin.tluczykont@physik.uni-hamburg.de
20 Tunka site exposure map Tunka site exposure map Field of view: π steradian
21 Tunka site exposure map H.E.S.S. SCAN HiSCORE scan normal mode Tunka site exposure map First H.E.S.S. Galactic plane scan Field of view: π steradian
22 Tunka site exposure map HiSCORE scan normal mode Detector axis Tilting
23 Tunka site exposure map H.E.S.S. SCAN HiSCORE scan normal mode Detector axis Tilting
24 Array optimization Simulation studies: Large PMTs (12'') Graded array layout
25 Physics Potential Tluczykont et al. (2014) 2014APh T
26 MGRO J Assuming pevatron with cutoff at 3PeV 10 km² No µ det. 1 year (200h)
27 Tycho Supernova remnant Assuming pevatron with cutoff at 3PeV 100 km² No µ det. 3 years
28 MGRO J2031 e+e pair production 100 TeV < 3% absorption Topic absorption most interesting for Multifrequency 3 PeV < 25% absorption CMB (A. Maurer DPG T )
29 e e pair production MGRO J2031 Topic absorption most interesting for Multifrequency conference! Many Galactic Universal feature: sources: Distance-dependent absorption Weak absorption up to 300TeV above 300TeV
30 The Tunka-HiSCORE project First realization of the HiSCORE concept
31 Helmholtz-Russia Joint Research Group HRJRG-303 Russian Mega-grant
32 Tunka-HiSCORE Tunka Cosmic ray experiment Tunka-133: 1 km² dense array Energy threshold 1015 ev Tunka-HiSCORE: 9-station array 25+stations martin.tluczykont@physik.uni-hamburg.de
33 Status 1st light prototype station array 2012/13 9-station array since October
34 Status Prototype-array: 9 stations, 300m X 300m 150m inter-station distance 4 channels (PMT+Cone) 2 parallel DAQ systems Gamma-ray energy threshold: <100TeV Future improvements: Graded array and clipping + 25 stations + IACTs martin.tluczykont@physik.uni-hamburg.de
35 Status Prototype-array: 9 stations, 300m X 300m 150m inter-station distance 4 channels (PMT+Cone) 2 parallel DAQ systems Gamma-ray energy threshold: <100TeV Future improvements: Graded array and clipping + 25 stations + IACTs martin.tluczykont@physik.uni-hamburg.de
36 Detector components
37 Optical station Electronic box
38 Detector components Alanod 4300UP reflective sheets 8'' PMTs (Hamamatsu & ElectronTubes)
39 9-station array DAQ Fan & Sum DRS4eb x2 White Rabbit (ethernet t-sync) RaspberryPI 9-channel DRS4 board Optical fiber carrier t-sync Central House PCs
40 9-station array DAQ Slow control system (High voltage, lid control, monitoring) Analog sum trigger: Σ i=1..4 a i > A thr Plan: clipped sum trigger (reduction of noise) 2 independent DRS4-based DAQ systems DRS4 custom board + t-sync system DRS4 evaluation board + WhiteRabbit sub-ns time- synchronization martin.tluczykont@physik.uni-hamburg.de Low threshold trigger GHz sampling and sub-ns precision!
41 RaspberryPI DRS4 WR FPGA TRIGGER INPUT Anodes Dynode Anode Sum
42 Detector components DRS4 ev.brd RaspberryPI Analog Summator Analog summator WhiteRabbit time synchr. System (Talk by A. Porelli) Onboard FPGA : triggering
43 Data quality Operation since 10/2013 Daily quality checks (rate stability, amplitude spectra, tie difference distributions,...)
44 Raw data Amplitude distributions
45 Noise and Cosmic triggers MC-Threshold
46 Timing verification CRs LED Pulsed LED Light source Spherical wave fit: sub-ns timing resolution
47 Combining HiSCORE with telescopes Non-imaging and imaging hybrid detection
48 HiSCORE + IACTs Central reconstruction parameter: Shower core position IACT image scaling Monoscopic operation Increased area / telescope martin.tluczykont@physik.uni-hamburg.de
49 HiSCORE + IACTs Central reconstruction parameter: Shower core position Simulation: sim_telarray IACT image scaling Monoscopic operation Increased area / telescope martin.tluczykont@physik.uni-hamburg.de
50 HiSCORE + IACTs sim_telarray martin.tluczykont@physik.uni-hamburg.de High Altitude Workshop 2014
51 Test width scaling with IACT+HiSCORE toy-mc-test Full simulation sim_telarray 2D-lookup-table for MC-width w MC (core, size) MC-core randomized with HiSCORE resolution Use randomized core position for width scaling martin.tluczykont@physik.uni-hamburg.de High Altitude Workshop 2014
52 HiSCORE + IACTs Preliminary results hybrid width scaling: Improves gamma-hadron separation Increases total area as compared to stereoscopic array PRELIMINARY Apply scaled width cut: Q-factor ~2.2 (Simulated granularity: 0.5 ) martin.tluczykont@physik.uni-hamburg.de
53 Hybrid events: more reconstruction Expect sensitivity boost: Scaled width cut (Q>2) Further g/h separation: Angular cut, length, (+ more sophisticated methods) Improved angular resolution from hybrid events: e.g. treat telescope as part of array (not yet simulated) Consider time-development of image independent direction reconstruction High Altitude Workshop 2014
54 Large zenith angle: outside HiSCORE viewcone gradient sim_telarray simulation, 2010 Core High Altitude Workshop 2014
55 Hybrid events: Sensitivity High Altitude Workshop 2014
56 Summary & outlook Tunka-HiSCORE 9-Station array: Operational since 10/2013 Data verification and analysis ongoing TAIGA, Tunka Area International Gamma-ray and cosmic ray Astrophysics 1 km² engineering array HiSCORE + imaging telescopes Expect 1 st physics results PAO Prototypes planned for deployment 2015
57 Outlook 2: HiSCORE at Pierre Auger Observatory Prototype in Hamburg
58 Outlook 2: HiSCORE at Pierre Auger Observatory Dual purpose: 1. Cross-calibration with PAO detectors 2. Fluorescence measurements using signal timing
59 2D-lookup-table PRELIMINARY / LOW STATISTICS martin.tluczykont@physik.uni-hamburg.de High Altitude Workshop 2014
60 HiSCORE + IACTs Assuming HiSCORE core resolution ~20m Apply scaled width cut: Q-factor ~2.2 (Simulated granularity: 0.5 ) martin.tluczykont@physik.uni-hamburg.de
61 Hadron rejection (width) and camera granularity This simulation Aharonian et al High Altitude Workshop 2014
62 First HiSCORE prototypes deployed Tunka-133 detector station FIRST LIGHT /2012
63 3 Station array 10/ /2013 TRG1 TRG2: WhiteRabbit 10/ /2013
64 3 Station array 10/ /2013 TRG1 TRG2: WhiteRabbit 10/ /2013
65 3 Station array 10/ / / /2013
66 3 Station array 10/ / / /2013
67 Absorption Absorption of gamma-rays by e+e- pair production with low energy photons (Moskalenko et al. 2006): Interstellar radiation field Cosmic Microwave Background
68 Lateral Cherenkov Photon Distribution
69 Lateral Cherenkov Photon Distribution Want large area Want a few stations In inner light pool ~ m spacing
70 Lateral Cherenkov Photon Distribution Want large area Want a few stations In inner light pool ~ m spacing Low photon density: Need large collector area 0.5 m² per station
71 The HiSCORE detector Picture: Serge Brunier m 150
72 Simulation & reconstruction CORSIKA + IACT *.iact sim_score iact-package Full detector sim *.ascii *.root reco_score
73 Simulation & Reconstruction
74 Reconstruction Major topic of PhD thesis, HiSCORE event display 500 TeV gamma-ray Simulation
75 Reconstruction Direction: photon arrival time model Energy: Value of 220 m Particle type: Shower depth and Signal rise-time
76 Reconstruction Extract PMT signal parameters Preliminary shower core position (cog) Preliminary direction (time plane fit) Improved core position: light distribution function (LDF) fitting Improved direction: arrival time model Fit of signal widths Simulated Cherenkov signal 05/26/14 High Altitude Workshop 2014
77 Direction reconstruction >3 stations: model fit adapted from Stamatescu et al. 2008, Parametrization of time-delay dt at detector position 05/26/14 High Altitude Workshop 2014
78 Direction reconstruction >3 stations: model fit adapted from Stamatescu et al. 2008, Parametrization of time-delay dt at detector position r: Distance from shower core to detector Shower height in km Slope of atmospheric refractive index Zenith angle 05/26/14 High Altitude Workshop 2014
79 Direction reconstruction 05/26/14 High Altitude Workshop 2014
80 Angular resolution of alternative layouts 05/26/14 High Altitude Workshop 2014
81 Energy reconstruction Particle energy: Q220 = Value of LDF at 220m Q220 05/26/14 martin.tluczykont@physik.uni-hamburg.de.de High Altitude Workshop 2014
82 Energy reconstruction Particle energy: Q220 = Value of LDF at 220m 05/26/14 martin.tluczykont@physik.uni-hamburg.de.de High Altitude Workshop 2014
83 Shower depth reconstruction Time model method: one free parameter in arrival time model LDF method: Depth from LDF slope, Q50/Q220 Width method: Depth from signal width 05/26/14 High Altitude Workshop 2014
84 Shower depth Depth of shower maximum 05/26/14 High Altitude Workshop 2014
85 Shower depth bias Systematic bias LDF & widths : sensitive to whole shower Large overestimation for heavy particles (long tails) Timing : sensitive to specific point (edge time) Small overestimation for heavy particles 05/26/14 martin.tluczykont@physik.uni-hamburg.de.de High Altitude Workshop 2014
86 Particle separation 05/26/14 High Altitude Workshop 2014
87 Particle separation (1) Lighter particles develop Higher up in atmosphere 05/26/14 High Altitude Workshop 2014
88 Particle separation (2) Systematic difference Between width and timing Depths 05/26/14 High Altitude Workshop 2014
89 Particle separation (3) Systematic difference Cherenkov signal rise times 05/26/14 High Altitude Workshop 2014
90 HRJRG-303 Helmholtz Russia Joint Research Group Measurements of Gamma Rays and Charged Cosmic Rays in the Tunka-Valley in Siberia by Innovative New Technologies 04/ /2015 G. Rubtsov, I. Tkatchev (INR) A. Konstantinov, L. Kuzmichev (MSU) HiSCORE and Radio Tunka R. Vasilyev, N. Budnev (ISU) R. Wischnewski, C. Spiering (DESY) F. Schröder, A. Haungs (KIT) M. Tluczykont, D. Horns (U. Hamburg) Innovation Proof-of-principle Synergies
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