Results of the Telescope Array experiment
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1 Results of the Telescope Array experiment Grigory I. Rubtsov Institute for Nuclear Research of the RAS ULB Physique Théorique seminar Bruxelles, February 4, G.I. Rubtsov Results of the Telescope Array experiment 1
2 Outline Telescope Array experiment TA physics results on UHECRs spectrum chemical composition search for sources search for photons Conclusions G.I. Rubtsov Results of the Telescope Array experiment 2
3 UHECR ground-based experiments, E ev G.I. Rubtsov Results of the Telescope Array experiment 3
4 Telescope Array Collaboration T Abu-Zayyad 1, R Aida 2, M Allen 1, R Azuma 3, E Barcikowski 1, JW Belz 1, T Benno 4, DR Bergman 1, SA Blake 1, O Brusova 1, R Cady 1, BG Cheon 6, J Chiba 7, M Chikawa 4, EJ Cho 6, LS Cho 8, WR Cho 8, F Cohen 9, K Doura 4, C Ebeling 1, H Fujii 10, T Fujii 11, T Fukuda 3, M Fukushima 9,22, D Gorbunov 12, W Hanlon 1, K Hayashi 3, Y Hayashi 11, N Hayashida 9, K Hibino 13, K Hiyama 9, K Honda 2, G Hughes 5, T Iguchi 3, D Ikeda 9, K Ikuta 2, SJJ Innemee 5, N Inoue 14, T Ishii 2, R Ishimori 3, D Ivanov 5, S Iwamoto 2, CCH Jui 1, K Kadota 15, F Kakimoto 3, O Kalashev 12, T Kanbe 2, H Kang 16, K Kasahara 17, H Kawai 18, S Kawakami 11, S Kawana 14, E Kido 9, BG Kim 19, HB Kim 6, JH Kim 6, JH Kim 20, A Kitsugi 9, K Kobayashi 7, H Koers 21, Y Kondo 9, V Kuzmin 12, YJ Kwon 8, JH Lim 16, SI Lim 19, S Machida 3, K Martens 22, J Martineau 1, T Matsuda 10, T Matsuyama 11, JN Matthews 1, M Minamino 11, K Miyata 7, H Miyauchi 11, Y Murano 3, T Nakamura 23, SW Nam 19, T Nonaka 9, S Ogio 11, M Ohnishi 9, H Ohoka 9, T Okuda 11, A Oshima 11, S Ozawa 17, IH Park 19, D Rodriguez 1, SY Roh 20, G Rubtsov 12, D Ryu 20, H Sagawa 9, N Sakurai 9, LM Scott 5, PD Shah 1, T Shibata 9, H Shimodaira 9, BK Shin 6, JD Smith 1, P Sokolsky 1, TJ Sonley 1, RW Springer 1, BT Stokes 5, SR Stratton 5, S Suzuki 10, Y Takahashi 9, M Takeda 9, A Taketa 9, M Takita 9, Y Tameda 3, H Tanaka 11, K Tanaka 24, M Tanaka 10, JR Thomas 1, SB Thomas 1, GB Thomson 1, P Tinyakov 12,21, I Tkachev 12, H Tokuno 9, T Tomida 2, R Torii 9, S Troitsky 12, Y Tsunesada 3, Y Tsuyuguchi 2, Y Uchihori 25, S Udo 13, H Ukai 2, B Van Klaveren 1, Y Wada 14, M Wood 1, T Yamakawa 9, Y Yamakawa 9, H Yamaoka 10, J Yang 19, S Yoshida 18, H Yoshii 26, Z Zundel 1 1 University of Utah, 2 University of Yamanashi, 3 Tokyo Institute of Technology, 4 Kinki University, 5 Rutgers University, 6 Hanyang University, 7 Tokyo University of Science, 8 Yonsei University, 9 Institute for Cosmic Ray Research, University of Tokyo, 10 Institute of Particle and Nuclear Studies, KEK, 11 Osaka City University, 12 Institute for Nuclear Research of the Russian Academy of Sciences, 13 Kanagawa University, 14 Saitama University, 15 Tokyo City University, 16 Pusan National University, 17 Waseda University, 18 Chiba University 19 Ewha Womans University, 20 Chungnam National University, 21 University Libre de Bruxelles, 22 University of Tokyo, 23 Kochi University, 24 Hiroshima City University, 25 National Institute of Radiological Science, Japan, 26 Ehime University
5 Telescope Array observatory 507 SD s, S = 3m 2 3 FD s CLF G.I. Rubtsov Results of the Telescope Array experiment 5
6 TA surface detector G.I. Rubtsov Results of the Telescope Array experiment 6
7 TA surface detector < Surface Detector > 200kg wlan (2.4GHz) solarpanel (120w) GPS scintillator box electronics box + battery (100Ah) WLSF: 1.0mmφ (2cm separation) PMTs: 3m 2 ET 9123SA 2 (12mm 2 layers) G.I. Rubtsov Results of the Telescope Array experiment 7
8 < SD Observation Status > Observation Time [hr] Observation Time [hr] Observation Time [hr] Mar 08 Nov 08 Nov 09 Feb 10 MJD M. Takeda, JPS meeting, March hrs operation in stable 97.5 % > 95% 10 > 16k hours Black Rock Mesa hrs 95.7 % Long Ridge hrs 94.2 % Smelter Knoll wlan interference in early stage thunder storms in summer maintenance access in autumn low temperature & snow in winter G.I. Rubtsov Results of the Telescope Array experiment 8
9 SD event example < SD Event Example > M. Takeda, JPS meeting, March Density [m ] Y [m] Core Distance [m] X [m] #FADC (raw) Td [nsec] Core Distance [m] RUN(50141) EVENT(2182) DATE(080531) TIME(050737) Log(E[eV])= η = Zenith=36.246[deg] Azimuth= [deg] Core(9) ChiD(0.09) ChiCS(1.39) Relative Timimg [nsec] G.I. Rubtsov Results of the Telescope Array experiment 9
10 G. Thomson, ICHEP 10, Paris
11 < FD Observation Status > Nov 07 Full operation since Nov 07 Feb 10 Observation Time [hr] Observation Time [hr] MJD May hrs 12.4 % Black Rock Mesa hrs 10.8 % Long Ridge Long Ridge remote operation since May 09 > 2.5k hrs > 2.1k hrs M. Takeda, JPS meeting, March 2010
12 FD event example Takeda, JPS meeting, March 2010 M.
13 Hybrid event example
14 < Atmospheric Monitor (LIDAR, CLF) & LINAC > back-scat. side-scat. LIDAR electron shower LINAC 40MeV 10 9 e (6.4mJ) CLF 100m 20.85km G.I. Rubtsov Results of the Telescope Array experiment 14
15 TA-LINAC: Linear TA I Electron accelerator 100 m from TA FD I Rate 0.5 Hz I Energy 40 MeV I Current pC/pulse T.Shibata, UHECR-2010, Nagoya Fist run: September 2010 G.I. Rubtsov Results of the Telescope Array experiment 15
16 T.Shibata, UHECR-2010, Nagoya
17 Telescope Array physics objectives Study of UHECR E ev Spectrum Chemical composition Search for sources Search for photons and neutrino Hadronic interactions properties G.I. Rubtsov Results of the Telescope Array experiment 17
18 TA physics results I. UHECR spectrum II. Chemical composition by XMAX stereo III. Search for cosmic ray sources IV. Search for photons G.I. Rubtsov Results of the Telescope Array experiment 18
19 TA physics results scheme G.I. Rubtsov Results of the Telescope Array experiment 19
20 I. UHECR spectrum G.I. Rubtsov Results of the Telescope Array experiment 20
21 GZK effect Greisen, 1966; Zatsepin, Kuzmin, 1966 Cut-off predicted for E ev. p + γ 2.7K n + π + p + π 0 AGASA spectrum, 2003 Takeda, M. et al., Astropart. Phys 19(2003) Expected 1.9 event Observed 11 events above ev G.I. Rubtsov Results of the Telescope Array experiment 21
22 Cut-off observation by HiRES Monocular: Quarks 06; PRL 100 (2008) Stereo: Astropart. Phys. 32 (2010) G.I. Rubtsov Results of the Telescope Array experiment 22
23 Pierre Auger spectrum PRL 101 (2008) & Phys. Lett. B 685 (2010) G.I. Rubtsov Results of the Telescope Array experiment 23
24 Telescope Array spectrum TA measures spectrum by three techniques: Middle Drum fluorescence detector (FD) mono Surface detector (SD) Hybrid (SD+FD) G.I. Rubtsov Results of the Telescope Array experiment 24
25 Monocular spectrum from Middle Drum (MD) detector MD uses 14 refurbish HiRes-1 telescopes. TAMD mono processing is identical to HiRes-1 monocular data analysis same program set same average atmospheric model same event selection, cuts Differences: telescope location and pointing directions Thresholds ( 20% lower than HiRes-1) Exposure is calculated with Monte-Carlo G.Thomson, ICHEP 10, Paris G.I. Rubtsov Results of the Telescope Array experiment 25
26 Jui, ICRC 2009 MD Spectrum 10 G.I. Rubtsov Results of the Telescope Array experiment 26
27 Surface detector spectrum Dataset: Geometrical cuts: θ < 45 core inside the array, distance to border > 1200 m Cuts on reconstruction quality: number of detectors hit >= 4 χ 2 /d.o.f < 4.0 pointing direction resolution < 5 fractional S800 uncertainty < years, 6264 events after cuts G.Thomson, ICHEP 10, Paris G.I. Rubtsov Results of the Telescope Array experiment 27
28 Energy scale normalization SD energy: CORSIKA QGSJET-II full MC FD energy: MD mono, BRM, LR hybrid Result: E = E SD /1.27 G.Thomson, ICHEP 10, Paris G.I. Rubtsov Results of the Telescope Array experiment 28
29 TA surface detector spectrum G.Thomson, ICHEP 10, Paris
30 GZK cut-off statistical significance G.Thomson, ICHEP 10, Paris
31 Surface detector, MD mono and hybrid spectra Note: SD energy normalized by 27% G.Thomson, ICHEP 10, Paris G.I. Rubtsov Results of the Telescope Array experiment 31
32 Comparison with AGASA, HiRes, Auger G.Thomson, ICHEP 10, Paris G.I. Rubtsov Results of the Telescope Array experiment 32
33 Spectrum summary Cut-off is observed by HiRES and confirmed by Pierre Auger and Telescope Array experiments GZK process in not questioned, but it s contribution to cut-off is unknown due to unknown spectrum and composition at the sources One may probe E > ev physics by looking at GZK secondaries: photons and neutrinos G.I. Rubtsov Results of the Telescope Array experiment 33
34 II. Chemical composition by XMAX stereo G.I. Rubtsov Results of the Telescope Array experiment 34
35 Auger/HiRES XMAX results Auger Phys.Rev.Lett ] 2 <X max> [g/cm QGSJET01 QGSJETII Sibyll2.1 EPOSv1.99 proton iron ] 2 ) [g/cm max RMS(X proton iron E [ev] E [ev] HiRES Phys.Rev.Lett G.I. Rubtsov Results of the Telescope Array experiment 35
36 Yakutsk array result on chemical composition EPOS p EPOS Fe 8 8 Number of events Number of events Ρ Μ obs Ρ Μ sim, p Ρ obs sim, Fe Μ Ρ Μ 0.29 ɛ Fe 0.68 (95%CL), E > ev Glushkov et al, JETP Letters 87: ,2008 G.I. Rubtsov Results of the Telescope Array experiment 36
37 Possible interpretation of Auger result The disappointing model Auger 09 Auger 09 E 3 J(E), ev 2 m -2 sec -1 ster rectilinear Kolm. diffusion protons E max =4 EeV =2.3, d=40 Mpc g E, ev E 3 J(E), ev 2 m -2 sec -1 ster rectilinear Kolm. diffusion protons E max =4 EeV =2.3, d=40 Mpc g nuclei E, ev R. Aloisio, V. Berezinsky, A. Gazizov arxiv: v1 No GZK-photons, no GZK-neutrino Will not see the sources G.I. Rubtsov Results of the Telescope Array experiment 37
38 Another interpretation of Auger result R. Engel, 31th ICRC, arxiv: v1 Auger, Phys.Rev.Lett ] 2 [gcm Mean X max 920 cross section 900 multiplicity 880 elasticity ] 2 [gcm RMS X max f 19 Protons with cross-section growth at high energies G.I. Rubtsov Results of the Telescope Array experiment 38
39 Auger/HiRES XMAX results Auger: Southern hemisphere Heavy nuclei or cross-section growth? HiRES: Northern hemisphere Protons dominate G.I. Rubtsov Results of the Telescope Array experiment 39
40 Telescope Array stereo result TA data favor protons data collection is in progress Y. Tameda, UHECR-2010, Nagoya G.I. Rubtsov Results of the Telescope Array experiment 40
41 TA XMAX distributions Y. Tameda, UHECR-2010, Nagoya G.I. Rubtsov Results of the Telescope Array experiment 41
42 TA XMAX distributions Y. Tameda, UHECR-2010, Nagoya G.I. Rubtsov Results of the Telescope Array experiment 42
43 III. Search for cosmic ray sources G.I. Rubtsov Results of the Telescope Array experiment 43
44 Pierre Auger AGN claim G.I. Rubtsov Results of the Telescope Array experiment 44
45 Auger claim discussion HiRES doesn t see correlations with AGN (2 of 13, bg: 3) Astropart.Phys.30,2008 Comment by Gorbunov,Tinyakov,Tkachev,Troitsky JETP Lett.87,2008 Events do not follow prediction of AGN hypothesis. E.g. nothing comes from Virgo, while it contains significant fraction of nearby AGNs Cen A may be a single source with correlation angle about 20 AGN correlation requires proton primaries; contradicts with Auger composition results due to large deflection of nuclei in Galactic magnetic field G.I. Rubtsov Results of the Telescope Array experiment 45
46 Pierre Auger claim discussion: Cen A Log 10 P distance from Cen A, deg The Monte-Carlo probability P to have the observed number of events in a circle of a given radius around Cen A on the celestial sphere, out of the 27 events of the Auger sample. Gorbunov,Tinyakov,Tkachev,Troitsky, arxiv: G.I. Rubtsov Results of the Telescope Array experiment 46
47 Auger AGN correlation update Pierre Auger collaboration, Astropart. Phys. 34 (2010) Before publication date: 9/13 correlate. Background: 2.7 ± 1.6 After publication date: 12/42 correlate. Background: 8.9 ± 3.0 G.I. Rubtsov Results of the Telescope Array experiment 47
48 Auger Centaurus A update Cen A may be a source Pierre Auger collaboration, Astropart. Phys. 34 (2010) Unfortunately out of field of view of HiRES and TA G.I. Rubtsov Results of the Telescope Array experiment 48
49 TA result on AGN correlation P.Tinyakov, UHECR-2010, Nagoya
50 TA result on AGN correlation correlate: 6 of 15, bg: 3.6 P.Tinyakov, UHECR-2010, Nagoya
51 TA Autocorrelation analysis P.Tinyakov, UHECR-2010, Nagoya
52 TA Autocorrelation analysis P.Tinyakov, UHECR-2010, Nagoya
53 TA correlations with LSS P.Tinyakov, UHECR-2010, Nagoya
54 TA correlations with LSS P.Tinyakov, UHECR-2010, Nagoya
55 TA LSS: result of the statistical tests P.Tinyakov, UHECR-2010, Nagoya
56 TA LSS: result of the statistical tests P.Tinyakov, UHECR-2010, Nagoya
57 Sources summary Correlations with AGN: 6/15 correlate; compatible with background; No significant clustering at E > 10 EeV and E > 40 EeV; Data with E > 40 EeV are compatible both with structure and isotropy; Data with E > 57 EeV are compatible with structure and incompatible with isotropy at 95% CL; G.I. Rubtsov Results of the Telescope Array experiment 57
58 IV. Search for photons G.I. Rubtsov Results of the Telescope Array experiment 58
59 Photon search techniques Photon-sensitive parameter: AGASA, Yakutsk muon density (strongest discrimination) Pierre Auger SD shower front curvature and thinkness Pierre Auger hybrid XMAX Telescope Array SD shower front curvature G.I. Rubtsov Results of the Telescope Array experiment 59
60 Shower front curvature deep shower maximum = curved front We use Linsley s shower front curvature parameter a as a composition sensitive parameter G.I. Rubtsov Results of the Telescope Array experiment 60
61 TA SD photon search Dataset: Data collected by SD from to Geometrical exposure for θ [θ 1, θ 2 ]: A geom = 2346 (sin 2 θ 2 sin 2 θ 1 ) km 2 sr yr Cuts for photon search: Number of detectors triggered is 7 or more Shower core distance to array boundary is larger than 1 separation unit (1200 m) χ 2 /d.o.f. < 5 G.I. Rubtsov Results of the Telescope Array experiment 61
62 Front curvature example Fit data Average photon front delay [1200m]; core distance [1200m] G.I. Rubtsov Results of the Telescope Array experiment 62
63 Linsley curvature a : data vs photon MC 0 30 h_gm h_gm h_gm h_dt h_gm h_dt Entries Entries Mean RMS Mean RMS Underflow Underflow Overflow Overflow a a h_gm h_dt Entries Mean RMS Underflow 0 Overflow E γ > ev data photon MC, E 2 spectrum a G.I. Rubtsov Results of the Telescope Array experiment 63
64 Event-by-event method For each event with curvature a obs we select photon MC events compatible by arrival direction and S 800. We calculate curvature distribution function f γ (a) for MC photons Let s define C = C is defined event-by-event a obs f γ (a)da For gamma events, C is uniformly distributed between 0 and 1 (independently of the photon primary spectrum). G.I. Rubtsov Results of the Telescope Array experiment 64
65 C: data vs photon MC h_gm h_dt Entries Mean RMS Underflow 0 Overflow h_gm h_dt Entries Mean RMS Underflow 0 Overflow C C h_gm h_dt Entries Mean RMS Underflow 0 Overflow E γ > ev data photon MC, E 2 spectrum C G.I. Rubtsov Results of the Telescope Array experiment 65
66 Calculations Search region: E gamma > ev 1395 events 45 < θ < events C > event Poisson 95% upper limit: 5.14 events Total exposure: A total = 158 km 2 sr yr F γ < km 2 sr 1 yr 1 (95% CL) /PRELIMINARY/ G.I. Rubtsov Results of the Telescope Array experiment 66
67 Photon flux limits 38 Log E 2 F Γ ev 2 km 2 yr 1 sr PRELIMINARY Y Y Y A TA ICRC TA PA PA A PA Log E min ev G.Rubtsov, JPS March 2010; Quarks 10 G.I. Rubtsov Results of the Telescope Array experiment 67
68 Photon fraction and flux limits Ε Γ,% Y Fraction limits PAO-H Y PAO-H Y HP A PAO-H PAO-H PAO-SD Log E min ev A Y PAO-SD A HP PAO-SD Y AH AY Log E 2 F Γ ev 2 km 2 yr 1 sr Flux limits PRELIMINARY Y Y Y Log E min ev A TA ICRC TA PA PA A PA GZK prediction: ɛ γ < 1% for E > ev Gelmini,Kalashev,Semikoz, JCAP 0711 (2007) Photons may be detected in the near future (depends on astrophysics parameters) G.I. Rubtsov Results of the Telescope Array experiment 68
69 Constraints on parameters of Superheavy dark matter Log 10 F SH m 2 sr 1 s Log 10 M X ev F SH flux of SHDM-produced cosmic rays E > ev above thick line excluded by spectral fits shaded area allowed by spectrum and γ limits SHDM decay may not be the source of all UHECRs Kalashev, Rubtsov, Troitsky, Phys.Rev.D80,2009 G.I. Rubtsov Results of the Telescope Array experiment 69
70 Lorentz invariance violation tests 1/2 LIV is proposed by Coleman & Glashow to suppress GZK process Phys.Rev.D59,1999 If LI is broken, threshold of GZK reaction may be upshifted p + γ 2.7K (1232) If we can prove that GZK reaction takes place, we have a constraint on LIV parameters One approach to confirm GZK reaction is to observe secondary photons These tests are strongest due to huge Lorentz factors. G.I. Rubtsov Results of the Telescope Array experiment 70
71 Lorentz invariance violation tests 2/2 If LI is broken for photons in form pair production on CMB ω 2 = k 2 + ξ n k 2 (k/m Pl ) n γ + γ CMB e + + e may be suppressed by kinematics and photons will propagate through large distances. Observed photon flux will contradict existing photon limits if ξ or ξ Galaverni, Sigl, Phys.Rev.Lett.100, 2008 Drawback: conclusion depends on the primary composition G.I. Rubtsov Results of the Telescope Array experiment 71
72 Conclusions TA is a large scale detector operating in the northern hemisphere Results on spectrum, composition and anisotropy are presented UHECR sources are not yet discovered Good chance to detect GZK photons in the midrange future (3-5 years) Photon discovery will highlight the highest energy processes G.I. Rubtsov Results of the Telescope Array experiment 72
73 Thank you! G.I. Rubtsov Results of the Telescope Array experiment 73
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