The HiSCORE Detector. HAP Topic 4 Workshop Jan th Rayk Nachtigall. Karlsruhe January 25th

Transcription

1 The HiSCORE Detector HAP Topic 4 Workshop Jan th 2013 Rayk Nachtigall Karlsruhe January 25th

2 Overview - Physics motivation - The HiSCORE detector - Signal processing - Physics potentials in γ-ray astronomy - Current state and plans 2

3 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 2011AdSpR T, astro-ph/ Large Field of view: ~ 0.6 sr

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 Tevatron sky TeV Gammarays: E > 100 GeV 7

8 Pevatron sky? Where are the cosmic ray pevatrons? 8

9 Accessing the pevatron sky: large area The HiSCORE detector 9

10 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 10 Picture: Serge Brunier

11 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 11 Picture: Serge Brunier

12 The HiSCORE detector Picture: Serge Brunier m

13 The HiSCORE detector Picture: Serge Brunier m

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

15 The HiSCORE detector 15

16 The HiSCORE detector WinstonControl Cone Station 10 segments of slow control with ALANODMEGA 4300 UP Arduino 2562 increase light collecting DAQ interface & station areaguruplug PC 4x 16

17 The HiSCORE detector 17

18 The HiSCORE detector Winston Cone 10 segments of ALANOD 4300 UP increase light collecting area 4x 18

19 The HiSCORE detector 19

20 The HiSCORE detector Winston ET 9352KB Cone 8 PMT with 6 stages 10 segments of 4 nominal gain kV 4300 UP PHQ9352 divider base increase lightwith collecting on area 4xHV generation board readout of anode & 5th dynode 20

21 The HiSCORE detector 21

22 The HiSCORE detector Winston Cone Readout trigger board with clipped-sum-trigger 10 segments of ALANOD 4300 UP DRS4 based sampling increase light collecting 1 GS/s area sampling 4x currently Evaluation Board V3 22

23 Further component alternatives & developments MSU trigger boards (DRS4 based in prep.) PMT & divider bases ISU box mechanics 23

24 Signal Processing 24

25 Signal Processing 25

26 Signal Processing 26

27 Signal Processing D. Hampf, PhD thesis 27

28 Signal Processing 28

29 Signal Processing 29

30 Signal Processing 30

31 Physics potential of HiSCORE (gamma-ray astronomy) 31

32 Opening the Pevatron range 32

33 Opening the Pevatron range IceCube HAWC CTA 33 LHAASO

34 Opening the Pevatron range 34

35 HiSCORE current status and plans 35

36 Helmholtz Russia Joint Research Group HRJRG U. Hamburg KIT Desy Zeuthen Hamburg Tunka Cosmic ray experiment INR Moscow MSU Moscow ISU Irkutsk 36

37 First HiSCORE prototype deployed HiSCORE prototype Tunka Tunka-133 detector station First HiSCORE Prototype April 2012 FIRST LIGHT 37

38 Helmholtz Alliance for Astroparticle Physics PAO letter of intent written, waiting for decision small array (5 stations) synergy with infill SD and FD expected 10 cross events per day from arxiv:

39 Summary & outlook HiSCORE goals: Ultra-high energy gamma-ray observation window Cosmic ray physics from 100 TeV to 1 EeV Particle physics beyond LHC energy range Activities: 3 stations since April 2012 small PAO 2013/14 Engineering array (1 km²), HiSCORE-EA: Start 2013 st Potential for 1 physics results 39

40 Thank you! 40

41 Backup slides 41

42 Tunka site exposure map Tunka site exposure map Field of view: π steradian 42

43 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 43 Field of view: π steradian

44 Tunka site exposure map 44 Det ect or axi st iltin g HiSCORE scan normal mode

45 Tunka site exposure map 45 Det ect or axi st iltin g H.E.S.S. SCAN HiSCORE scan normal mode

46 Reconstruction Extract PMT signal parameters Preliminary shower core position (cog) Preliminary direction (time plane fit) 46 Improved core position: light distribution function (LDF) fitting Improved direction: arrival time model Fit of signal widths Simulated Cherenkov signal

47 Direction reconstruction >3 stations: model fit adapted from Stamatescu et al. 2008, Parametrization of time-delay dt at detector position 47

48 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 48

49 Direction reconstruction 49

50 Energy reconstruction Particle energy: Q220 = Value of LDF at 220m Q220 50

51 Energy reconstruction 51 Particle energy: Q220 = Value of LDF at 220m

52 Cosmic rays Adapted from Donato & Medina-Tanco 2008 Gammas from Galactic Cosmic rays: Eγ ~ ECR/10 52

53 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 53

54 Shower depth 54 Depth of shower maximum

55 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 55

56 Particle separation 56

57 Particle separation (1) Lighter particles develop Higher up in atmosphere 57

58 Particle separation (2) Systematic difference Between width and timing Depths 58

59 Particle separation (3) Systematic difference Cherenkov signal rise times 59

60 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 60 Picture: Serge Brunier

61 Lateral Cherenkov Photon Distribution 61

62 Lateral Cherenkov Photon Distribution Want large area Want a few stations In inner light pool ~ m spacing 62

63 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 63

64 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) 64 HiSCORE and Radio Tunka Innovation Proof-of-principle Synergies

65 Helmholtz Russia Joint Research Group HRJRG 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 65

66 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] 66 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