HiSCORE. M. Tluczykont for the HiSCORE Collaboration

Transcription

1 Measurements of Gamma Rays and Charged Cosmic Rays in the Tunka-Valley in Siberia by Innovative New Technologies HRJRG 303 Sky above Tunka valley HiSCORE Detector Taiga Frozen Irkut river Irkut river HiSCORE M. Tluczykont for the HiSCORE Collaboration Fall meeting of the Astronomische Gesellschaft Splinter on Multi-Messenger Astroparticle Physics, RX J1713 H.E.S.S. gamma-rays

2 HiSCORE The Hundred*i Square-km Cosmic ORigin Explorer Cosmic-rays: 100 TeV < EC R < 1 EeV Gamma-rays: Eγ > 10 TeV, up to PeV, ultra-high energy regime Particle physics: beyond LHC range Concept: non-imaging air Cherenkov technique Large area: up to few 100 km² Large Field of view: ~ 0.6 sr AdSpR T, astro-ph/

3 Why do we need a large area? Energetic events are rare. 3

4 Physics motivations 4

5 ara ys Physics motivations spectroscopy Anisotropies G am m Gamma-ray spectra Highest and morphology acceleration energies Diffuse Gamma-ray Diffuse emission Emission (Galaxy, local supercluster) C os m Cosmic-ray Origin of cosmic Origin of rays cosmic rays Nonstandard Propagation Propagation Cosmic-ray Anisotropy Sub-knee pre-ankle Spectral fine-structure NucleonNucleon interaction Particle acceleration Dark matter Particle physics 5 ic -r ay s

6 Cosmic rays HiSCORE Adapted from Donato & Medina-Tanco 2008 Spectrum&composition in transition range Galactic / extragalactic origin 6

7 Cosmic ray origin Adapted from Donato & Medina-Tanco 2008 Gammas from Galactic Cosmic rays: Eγ ~ ECR/10 7

8 Tevatron sky TeV Cosmic rays Eγ > 100 GeV 8

9 Pevatron sky TeV Cosmic rays Eγ > 100 TeV? Where are the cosmic ray pevatrons? 9

10 The Pevatron energy range? 10

11 Opening the Pevatron range Extend energy range! very large area 11

12 Opening the Pevatron range Extend energy range! very large 100 TeV: hard hadronic spectra vs. soft leptonic spectra = cosmic ray signature 12

13 Accessing the pevatron sky: large area The HiSCORE detector 13

14 The HiSCORE detector How to achieve large effective area? Imaging air Cherenkov telescopes: O(1000) channels / km² Non-imaging air Cherenkov technique: O(100) channels / km² 14 Picture: Serge Brunier

15 The HiSCORE detector How to achieve large effective area? Imaging air Cherenkov telescopes: O(1000) channels / km² Non-imaging air Cherenkov technique: O(100) channels / km² Air shower Cherenkov light cone 15 Picture: Serge Brunier

16 The HiSCORE detector Lateral Cherenkov Photon Distribution How to achieve large effective area? Imaging air Cherenkov telescopes: O(1000) channels / km² Non-imaging air Cherenkov technique: O(100) channels / km² Air shower Cherenkov light cone 16 Picture: Serge Brunier

17 Lateral Cherenkov Photon Distribution 17

18 Lateral Cherenkov Photon Distribution Want large area Want a few stations In inner light pool ~ m spacing 18

19 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 19

20 The HiSCORE detector Picture: Serge Brunier m

21 The HiSCORE detector Picture: Serge Brunier m

22 The HiSCORE detector >0.5 m² station area: E thr Readout: GHz sampling <1ns time synch. Picture: Serge Brunier m

23 Physics potential of HiSCORE (gamma-ray astronomy) 23

24 Opening the Pevatron range 24

25 Opening the Pevatron range CTA 25

26 Opening the Pevatron range 26

27 Opening the Pevatron range 27

28 Potential HiSCORE detections H.E.S.S. (Veritas) 28

29 Tunka site exposure map Tunka site exposure map Field of view: π steradian 29

30 Tunka site exposure map HiSCORE scan, 1 year H.E.S.S. SCAN First H.E.S.S. Galactic plane scan 30 Tunka site exposure map Field of view: π steradian

31 HiSCORE current status and plans 31

32 Tunka valley Hamburg Tunka Cosmic ray experiment 1 km² dense array Energy threshold 1015 ev core position resolution ~ 10 m energy resolution ~ 15% Xmax resolution< 25 g cm-2 32

33 HRJRG-303 Helmholtz Russia Joint Research Group HRJRG-303 Measurements of Gamma Rays and Cosmic Rays in the Tunka-Valley in Siberia by innovative new technologies Low energy (GeV / TeV / PeV): High energy (PeV - EeV): HRJRG-303: Resolve open questions of cosmic rays With innovative methods Cherenkov Radio Cherenkov light cone HiSCORE 33 TunkaRex

34 HiSCORE Tunka HiSCORE prototype Tunka Top view: light sensors Tunka-133 detector station 34 First HiSCORE Prototype April 2012

35 HiSCORE Tunka S. Epimakhov HiSCORE prototype 35

36 Time synchronization WhiteRabbit: PTP over synchronuous ethernet Synergies: CTA & HiSCORE same t-synch. geometry Consistent lab & Tunka field-test results: sub-ns resolution T-synchronization Over 2 km ethernet rms ~0.17ns Stability LabTest 50 hrs R. Wischnewski 36

37 Plans 2012: further prototype deployments 2013: engineering array (~60 stations) 37 Proof-of principle & optimization Potentially first physics: strong pevatrons ~2015: 10 km² 100 km² Low-energy core (8'' 12'' PMTs) Optimized layout: graded? Possible combination with imaging technique Better overlap with Gamma: CTA C.R.: direct measurements

38 Summary & outlook HiSCORE goals: Ultra-high energy gamma-ray survey: pevatron search Cosmic ray physics from 100 TeV to 1 EeV Particle physics beyond LHC energy range Prototype activities Tunka (also planned later: PAO) Engineering array (1 km²), HiSCORE-EA: Start 2013 st Potential for 1 physics results 10 km² 100 km² ~2014 Southern site? 38

39 Recent news article: Upcoming publication: Tluczykont et al. 2012, The HiSCORE detector Submitted to Astroparticle physics 39

40 Opening the Pevatron range 40

41 Backup slides 41

42 Tunka site exposure map Det ect or axi st iltin g HiSCORE scan normal mode 42

43 Tunka site exposure map Det ect or axi st iltin g H.E.S.S. SCAN HiSCORE scan normal mode 43

44 Simulation & Reconstruction 44

45 Simulation & reconstruction CORSIKA + IACT *.iact sim_score iact-package Full detector sim *.ascii *.root reco_score 45

46 Reconstruction HiSCORE event display 500 TeV gamma-ray Simulation 46

47 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 47

48 Direction reconstruction >3 stations: model fit adapted from Stamatescu et al. 2008, Parametrization of time-delay dt at detector position 48

49 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 49

50 Reconstruction 50 Direction: photon arrival time model Energy: Value of 220 m Particle type: Shower depth and Signal rise-time

51 Direction reconstruction 51

52 Energy reconstruction Particle energy: Q220 = Value of LDF at 220m Q220 52

53 Energy reconstruction 53 Particle energy: Q220 = Value of LDF at 220m

54 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 54

55 Shower depth 55 Depth of shower maximum

56 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 56

57 Particle separation 57

58 Particle separation (1) Lighter particles develop Higher up in atmosphere 58

59 Particle separation (2) Systematic difference Between width and timing Depths 59

60 Particle separation (3) Systematic difference Cherenkov signal rise times 60

61 Layout studies Different altitudes Different PMT sizes Combination with other techniques (scintillator, imaging) 61

62 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) R. Vasilyev, N. Budnev (ISU) R. Wischnewski, C. Spiering (DESY) F. Schröder, A. Haungs (KIT) M. Tluczykont, D. Horns (U. Hamburg) 62 HiSCORE and Radio Tunka Innovation Proof-of-principle Synergies

63 References [HS1] [HS2] [HS3] [HS4] [HS5] [HS6] M. Tluczykont, D. Hampf, D. Horns, et al. (2011), Adv. Sp. Res. 48, 1935 D. Hampf (2012), PhD thesis, University of Hamburg M. Tluczykont, T. Kneiske, D. Hampf & D. Horns (2009), Proc. of the ICRC 2009, arxiv e-print (arxiv: v1) D. Hampf, M. Tluczykont & D. Horns (2009), Proc. of the ICRC 2009, arxiv e-print (arxiv: v1) M. Tluczykont, D. Hampf, D. Horns, et al., HiSCORE, in prep. D. Hampf, M. Tluczykont, D. Horns, HiSCORE reco, in prep. [Tunka133] Berezhnev S F, Besson D, Korobchenko A V et al The Tunka-133 EAS Cherenkov light array: status of 2011 NIM A DOI : /j.nima Preprint astro-ph.he/ [Hec1998] [Ber2008] [Hen1994] [Hör2003] [Abd2007] 63 D. Heck, J. Knapp, J.N. Capdevielle, G. Schatz, and T. Thouw, Report FZKA 6019 (1998), K. Bernlöhr (2008), astrop-ph preprint, arxiv: V. Henke (1994), Diploma thesis, University of Hamburg J.R. Hörandel, Astropart. Phys., 19, 193 (2003) Abdo A A, Allen B, Berley D et al Astrophys. J. 658 L33 L36