Highlights from the Telescope Array Experiment

Transcription

1 33 rd International Cosmic Ray Conference, Rio de Janeiro 2013 Highlights from the Telescope Array Experiment Hiroyuki Sagawa (ICRR, Univ. of Tokyo) for the Telescope Array Collaboration July 4,

2 Outline Telescope Array (TA) detector TA results Energy spectrum Composition anisotropy TA Extensions TA+Auger joint research 2

3 14 telescopes TA detector in Utah 39.3 N, W ~1400 m a.s.l. Refurbished HiRes Middle Drum (MD) 3 com. towers Surface Detector (SD) 507 plastic scintillator SDs 1.2 km spacing 700 km 2 Long Ridge (LR) 12 telescopes Fluorescence Detector(FD) 3 stations 38 telescopes 12 telescopes Black Rock Mesa (BR) 3

4 14 telescopes TA detector in Utah 39.3 N, W ~1400 m a.s.l. Refurbished HiRes Middle Drum (MD) 3 com. towers Surface Detector (SD) 507 plastic scintillator SDs 1.2 km spacing 700 km 2 Long Ridge (LR) 12 telescopes Observation 3 FD stations: Nov., 2007~ Hybrid (FD+SD): May, 2008~ Fluorescence Detector(FD) 3 stations 38 telescopes 12 telescopes Black Rock Mesa (BR) 4

5 14 telescopes TA detector in Utah 39.3 N, W ~1400 m a.s.l. Refurbished HiRes Middle Drum (MD) 3 com. towers Surface Detector (SD) 507 plastic scintillator SDs 1.2 km spacing 700 km 2 CLF Long Ridge (LR) 12 telescopes ELS Fluorescence Detector(FD) 3 stations 38 telescopes 12 telescopes Black Rock Mesa (BR) 5

6 Telescope Array Collaboration T. Abu-Zayyad a, M. Allen a, R. Anderson a, R. Azuma b, E. Barcikowski a, J. W. Belz a, D. R. Bergman a, S. A. Blake a, R. Cady a, M. J. Chae c, B. G. Cheon d, J. Chiba e, M. Chikawa f, W. R. Cho g, T. Fujii h, M. Fukushima h,i, K. Goto j, W. Hanlon a, Y. Hayashi j, N. Hayashida k, K. Hibino k, K. Honda l, D. Ikeda h, N. Inoue m, T. Ishii l, R. Ishimori b, H. Ito n, D. Ivanov a,o, C. C. H. Jui a, K. Kadota p, F. Kakimoto b, O. Kalashev q, K. Kasahara r, H. Kawai s, S. Kawakami j, S. Kawana m, K. Kawata h, E. Kido h, H. B. Kim d, J. H. Kim a, J. H. Kim d, S. Kitamura b, Y. Kitamura b, V. Kuzmin q, Y. J. Kwon g, J. Lan a, J.P. Lundquist a, K. Machida l, K. Martens i, T. Matsuda t, T. Matsuyama j, J. N. Matthews a, M. Minamino j, K. Mukai l, I. Myers a, K. Nagasawa m, S. Nagataki n, T. Nakamura u, H. Nanpei j, T. Nonaka h, A. Nozato f, S. Ogio j, S. Oh c, M. Ohnishi h, H. Ohoka h, K. Oki h, T. Okuda v, M. Ono n, A. Oshima j, S. Ozawa r, I. H. Park w, M. S. Pshirkov x, D. C. Rodriguez a, G. Rubtsov q, D. Ryu y, H. Sagawa h, N. Sakurai j, A. L. Sampson a, L. M. Scott o, P. D. Shah a, F. Shibata l, T. Shibata h, H. Shimodaira h, B. K. Shin d, T. Shirahama m, J. D. Smith a, P. Sokolsky a, R. W. Springer a, B. T. Stokes a, S. R. Stratton a,o, T. A. Stroman a, M. Takamura e, A. Taketa z, M. Takita h, Y. Tameda k, H. Tanaka j, K. Tanaka aa, M. Tanaka t, S. B. Thomas a, G. B. Thomson a, P. Tinyakov q,x, I. Tkachev q, H. Tokuno b, T. Tomida ab, S. Troitsky q, Y. Tsunesada b, K. Tsutsumi b, Y. Uchihori ac, F. Urban x, G. Vasiloff a, Y. Wada m, T. Wong a, H. Yamaoka t, K. Yamazaki j, J. Yang c, K. Yashiro e, Y. Yoneda j, S. Yoshida s, H. Yoshii ad, R. Zollinger a, Z. Zundel a a University of Utah, b Tokyo Institute of Technology, c Ewha Womans University, d Hanyang University, e Tokyo University of Science, f Kinki University, g Yonsei University, h Institute for Cosmic Ray Research, Univ. of Tokyo, i Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo, j Osaka City University, k Kanagawa University, l Univ. of Yamanashi, m Saitama University, n Astrophysical Big Bang Laboratory, RIKEN, o Rutgers University, p Tokyo City University, q Institute for Nuclear Research of the Russian Academy of Sciences, r Waseda University, s Chiba University, t Institute of Particle and Nuclear Studies, KEK, u Kochi University, v Ritsumeikan University, w Sungkyunkwan University, x Universite Libre de Bruxelles, y Chungnam National University, z Earthquake Research Institute, University of Tokyo, aa Hiroshima City University, ab Advanced Science Institute, RIKEN, ac National Institute of Radiological Science, ad Ehime University 6

7 Telescope Array Collaboration T. Abu-Zayyad a, M. Allen a, R. Anderson a, R. Azuma b, E. Barcikowski a, J. W. Belz a, D. R. Bergman a, S. A. Blake a, R. Cady a, M. J. Chae c, B. G. Cheon d, J. Chiba e, M. Chikawa f, W. R. Cho g, T. Fujii h, M. Fukushima h,i, K. Goto j, W. Hanlon a, Y. Hayashi j, N. Hayashida k, K. Hibino k, K. Honda l, D. Ikeda h, N. Inoue m, T. Ishii l, R. Ishimori b, H. Ito n, D. Ivanov a,o, C. C. H. Jui a, K. Kadota p, F. Kakimoto b, O. Kalashev q, K. Kasahara r, H. Kawai s, S. Kawakami j, S. Kawana m ~120, K. Kawata collaborators h, E. Kido h, H. B. Kim d, in J. H. 5 Kimcountries a, J. H. d, S. Kitamura b, Y. Kitamura b, V. Kuzmin q, Y. J. Kwon g, J. Lan a, J.P. Lundquist a, K. Machida l, K. Martens i, T. Matsuda t, T. Matsuyama j, J. N. Matthews a, M. Minamino Japan, j, K. Mukai USA, l, I. Korea, Myers a, K. Nagasawa Russia, m, S. Belgium Nagataki n, T. Nakamura u, H. Nanpei j, T. Nonaka h, A. Nozato f, S. Ogio j, S. Oh c, M. Ohnishi h, H. Ohoka h, K. Oki h, T. Okuda v, M. Ono n, A. Oshima j, S. Ozawa r, I. H. Park w, M. S. Pshirkov x, D. C. Rodriguez a, G. Rubtsov q, D. Ryu y, H. Sagawa h, N. Sakurai j, A. L. Sampson a, L. M. Scott o, P. D. Shah a, F. Shibata l, T. Shibata h, H. Shimodaira h, B. K. Shin d, T. Shirahama m, J. D. Smith a, P. Sokolsky a, R. W. Springer a, B. T. Stokes a, S. R. Stratton a,o, T. A. Stroman a, M. Takamura e, A. Taketa z, M. Takita h, Y. Tameda k, H. Tanaka j, K. Tanaka aa, M. Tanaka t, S. B. Thomas a, G. B. Thomson a, P. Tinyakov q,x, I. Tkachev q, H. Tokuno b, T. Tomida ab, S. Troitsky q, Y. Tsunesada b, K. Tsutsumi b, Y. Uchihori ac, F. Urban x, G. Vasiloff a, Y. Wada m, T. Wong a, H. Yamaoka t, K. Yamazaki j, J. Yang c, K. Yashiro e, Y. Yoneda j, S. Yoshida s, H. Yoshii ad, R. Zollinger a, Z. Zundel a a University of Utah, b Tokyo Institute of Technology, c Ewha Womans University, d Hanyang University, e Tokyo University of Science, f Kinki University, g Yonsei University, h Institute for Cosmic Ray Research, Univ. of Tokyo, i Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, the University of Tokyo, j Osaka City University, k Kanagawa University, l Univ. of Yamanashi, m Saitama University, n Astrophysical Big Bang Laboratory, RIKEN, o Rutgers University, p Tokyo City University, q Institute for Nuclear Research of the Russian Academy of Sciences, r Waseda University, s Chiba University, t Institute of Particle and Nuclear Studies, KEK, u Kochi University, v Ritsumeikan University, w Sungkyunkwan University, x Universite Libre de Bruxelles, y Chungnam National University, z Earthquake Research Institute, University of Tokyo, aa Hiroshima City University, ab Advanced Science Institute, RIKEN, ac National Institute of Radiological Science, ad Ehime University 7

8 Energy spectrum 8

9 TA shower analysis with FD An example of an air shower the camera view Longitudinal shower profile Cherenkov Systematic uncertainty in energy determination Fluorescence yeild 11% Atmospheric attenuation 11% Absolute detector calib. 10% reconstruction 10% total 21% Poster, 358 9

10 Poster, 395 TA shower analysis with SD An SD hit map of a typical high energy event Time fit Lateral distribution profile fit 10

11 Poster, 395 TA shower analysis with SD An SD hit map of a typical high energy event Time fit Geometry Zenith angle: θθ Azimuth angle S800 Lateral distribution profile fit 800 m 11

12 First estimation of SD energy Monte Carlo Energy table E SD = E SD (S800, θ) log 10 (S800) sec(θ) 2013/4/25 H. Sagawa 12

13 Energy Scale Check and resolution FD energy E FD Hybrid events E > ev Angular resolution = 1.4 o SD energy E SD (scaled to FD energy) EE SSSS = EE SSSS/1.27 E > ev Energy resolution < 20% 13

14 5 year TA SD spectrum TA data May, 2008 May, Zenith angle < 45 o ev. (E > ev) Exposure 4500 km 2 sr yr Broken power law fit 14

15 Significance of suppression 15

16 TA spectra by other methods Monocular FD BR/LR mono (3.5 yr) arxiv: , appear in APP Icrc poster, 476 MD mono APP 39 (2012) 109 Hybrid BR/LR hybrid arxiv: Icrc poster, 358 MD hybrid Icrc poster,

17 Spectrum overview D. Bergman, oral,

18 Mass Composition Photons, Neutrinos 18

19 FD stereo Xmax Pster, year data (Nov., 2007 Nov. 2011) Data: TA Red histogram: QGSJET-II proton model Blue histogram: QGSJET-II iron model The TA data is consistent with QGSJET-II proton prediction. 19

20 FD stereo Xmax 20

21 Hybrid Xmax analysis M. Allen, poster 794 MD FD + SD, 4 yrs 21

22 Photon search G. Rubtsov, oral 149 Hadron induced gamma indueced TA data Gamma MC 22

23 Neutrino search G. Rubtsov, oral

24 Anisotropy TA 5-year SD data 24

25 Correlations with AGN P. Tinyakov, oral, AGN from 2006 Veron catalog with z < E > 57 EeV, zenith angle < 45 o, N = 42 (5 yr) Separation angle = 3.1 o 25

26 Correlations with AGN Probability to hit AGN with a single event p o = events correlate out of 42 p =

27 Correlations with LSS P. Tinyakov, oral, 1033 E > 10 EeV: 2130 ev. E > 40 EeV: 132 ev. E > 57 EeV: 52 ev. White dots: TA data with zenith angle < 55 o Gray patterns: expected flux density from proton LSS 2MASS Galaxy Redshift catalog (XSCz) 27

28 Correlations with LSS E > 10 EeV E > 40 EeV E > 57 EeV Theta: deflection angle ~3σ (pre-trial) 28

29 P. Tinyakov, oral, 1033 Autocorrelations P(δ): The probability that the excess of pairs (<δ) occurs in a uniform distribution Small P(δ): departure from isotropy Separation angle P(δ)~0.004 at δ~20 o for E > 57 EeV 29

30 Super galactic coordinates KS p-value = 0.06 KS p-value =

31 Electron Light Source (ELS) T. Shibata, oral 507 An image of data Measured with FD Electron beam BR FD station 100m Cosmic ray Electron beam 40-MeV, 10 9 electrons (typical) End-to-end FD energy calibration 31

32 ELS analysis Real data ELS Energy/beam current from monitor FADC counts from FD Longitudinal distribution MC data Shower generation Geant4.9.5 or FD simulation TA official software Lateral distribution Data/MC agreement: within 5% Good agreement 32

33 Measurement of fluorescence yield by ELS Measured FY = Data MC( Air condition) [model dep. FY ( Air condition)] Measured average fluorescence yield (<measured FY>) The case of TA fluorescence yield (TA-FY) model Spectrum: FLASH model, Astropart Physics 29 (2008) Absolute yield: Kakimoto et al., NIM-A 372 (1996) <mmmmmmmmmmmmmmmm FFFF> = 1.18±0.01 ssssssss ± 0.18 ssssssss TTTT FFFF The case of common model CM-FY2012 Spectrum: B. Keihauer et al., Proc. UHECR2012, arxiv:astroph/ Absolute yield: AirFly meas. chosen here, arxiv: [astro-ph.im] <mmmmmmmmmmmmmmmm FFFF> = 0.96±0.01 ssssssss ± 0.15 ssssssss CCCC FFFF

34 TA physics result Type Title Primary author Energy spectrum Composition Arrival direction MD hybrid spectrum and composition M. Allen P 794 BR/LR hybrid spectrum D. Ikeda P 358 BR/LR mono spectrum T.A. Stroman P 476 O/P id Data Spectrum summary D. Bergman O 221 Jul 4 Spectrum interpretation E. Kido O 136 Jul 4 UHE photon and n with FD K. Yamazaki P 524 UHE photon and n with SD G. Rubtsov O 149 Jul 7 MD hybrid spectrum and composition M. Allen P 794 Stereo FD Xmax Y. Tameda P 512 SD composition S. Troitsky P 536 BR/LR hybrid composition W. Hanlon P 965 Composition summary Y. Tsunesada O 132 Jul 6 LE point-like sources K. Kawata P 310 LE LSS anisotropy K. Kawata P 311 Correlations with extragalactic objects H. Tokuno P 133 HE LSS anisotropy P. Tinyakov P 935 Anisotropy summary P. Tinyakov O 1033 Jul7 34

35 Some others Monte Carlo, calibrations, monitors type title Primary author P/ O Data/MC simulation Calibration/Monitoring Hadron interaction model and TA SD data TALE hybrid simulation and analysis id Date time B. Stokes O 353 July 3 T. AbuZayyad P 389 Shower front structure N. Sakurai P 130 FD calibration with ELS T. Shibata O 507 July 3 Atmospheric monitoring system YAP/Xe flasher for FD PMT camera monitoring S. Udo P 142 B.K. Shin P 952 trigger Hybrid trigger H. Tokuno P

36 TA extensions TALE, other R&D and plans type title Primary author P/O id Date TA general G. B. Thomson P 118 TA next 5 years H. Sagawa P 121 TALE S. Ogio O 717 July 3 TALE simulation D. Ivanov P 389 Status, plan NICHE J. Krizmanic O 365 July 3 Shower Universality for NICHE D. Bergma P 983 TARA J. Belz O 1192 July 4 Radio echo detection from ELS D. Ikeda P 360 TARA: CR radar echo I. Meyers P 639 Surface muon detector T. Nonaka P

37 S. Ogio et al., oral 717 T. Abu-Zayyad et al., poster 389 TALE (TA Low-energy Extension) E = ev Second knee at ~ ev? Drastic change of composition at ~10 18 ev? Transition from galactic to extra-galactic cosmic rays? ~10 17 ev cosmic ray shower: compatible with LHC centerof-mass energy 37

38 38

39 TALE (TA Low-energy Extension) 10 TALE FDs: refurbished HiRes-II telescopes installed and running. TALE SDs 35 TALE SDs were deployed among 101 SDs. 16 in operation TALE FD events (data) 39

40 NICHE project J. Krizmanic et al., oral 365 D. Bergman et al. poster 983 Non-Imaging CHErenkov Array (NICHE) TA/TALE extension to measure the the energy and composition (Xmax) of very-high energy cosmic rays E = to ev Proposed but not yet funded PMTs looking upwards Cherenkov counters within TALE infill array 40

41 TARA (TA Radar) J. Belz et al., oral 1192 I. Meyer et al., poster An R&D project to observe radar reflections form cosmic ray air showers TARA1.5 April 2011 to July kw TARA40 Summer 2013~ kw 41

42 H. Sagawa et al., poster 121 TA 4 A project to expand the TA surface detector by a factor of 4 (~3000 km 2 ) 500 more scintillation counters with 2.08 km spacing A fluorescence detector of 10 telescopes from HiRes telescopes The proposal is being prepared for submission in fall, Anisotropy studies with more significance By March, TA years of SD data 14 TA years of hybrid data 42

43 TA/Auger joint research type title Primary author P/O id Date Octocopter light source test J. N. Matthews O 1218 July 3 Joint research Octocopter light source test K. Honda P 504 Composition W. Hanlon O 964 July 6 anisotropy O. Deligny (Auger) O

44 Light Source Test J.N.Matthes et al., oral 1218 K. Machida et al., poster 504 A joint calibration campaign for the fluorescence telescopes Optical end-to-end calibration with a portable calibrated light source carried by an octocopter provided by Auger Known position: GPS Light source 1 km away Data with TA FD 44

45 Full-sky anisotropy analysis O. Deligny for the Telescope Array and the Pierre Auger Collaboration, oral Large-scale anisotropy at TA and Auger for E > ev Any anisotropy fingerprint is encoded in the set of spherical harmonics coefficients Partial coverage degrades the resolution require full coverage A method to obtain full-sky coverage by combining data sets from different observatories 45

46 Xmax analysis of an adhoc data compatible with Auger composition model via TA reconstruction Auger Xmax result ad hoc composition model (p, helium, nitrogen, iron) TA detector simulation and reconstruction W.F. Hanlon for TA and Auger collaboration Oral, 964 How well can the TA SD detector distinguish between Auger mixed composition and pure proton compositions? 46

47 Summary Five-year TA operation Recent results Energy spectrum Significance of the suppression 5.7σσ at ± ev Composition Consistent with proton Anisotropy Hints of anisotropy TA extensions TALE has started (10 full FDs, SD array partially) TA+Auger joint research to understand the results from TA and Auger 47