P. Tinyakov 1,2 TELESCOPE ARRAY: LATEST RESULTS. P. Tinyakov. for the Telescope Array Collaboration. Telescope Array detector.

Transcription

1 1,2 1 Université Libre de Bruxelles, Bruxelles, Belgium 2 Institute for Nuclear Research, Moscow, Russia Telescope

2 Outline Telescope Telescope

3 UHECR ground-based experiments Telescope

4

5 ARRAY DETECTOR Telescope

6 ARRAY HYBRID DETECTOR Telescope 507 scintillator s covering 680 km 2 3 fluorescence sites, 38 telescopes Surface fully operational from March 2008 SD relative size: TA 9 AGASA PAO/4

7 TA surface s Telescope Deployed with the spacing 1.2 km Powered by solar panels. Connected by radio.

8 Telescope

9 Hybrid event example Telescope

10 SPECTRUM Telescope

11 TA spectrum TA measures spectrum by three techniques: Middle Drum fluorescence (FD-mono) Surface (SD) Hybrid (SD+FD) Telescope

12 FD-mono spectrum Telescope

13 Surface spectrum Dataset: Geometrical cuts: θ < 45 core inside the array, distance to border > 1200 m Cuts on reconstruction quality: number of s hit 4 χ 2 /d.o.f < 4.0 pointing direction resolution < 5 fractional S 800 uncertainty < years, 6264 events after cuts Telescope

14 TA surface spectrum Telescope

15 SD, FD-mono and hybrid spectra Telescope Note: SD energy normalized by 27% down

16 Comparison with other experiments Telescope

17 CHEMICAL COMPOSITION Telescope

18 Telescope stereo result Telescope TA data favor protons [Y. Tameda, UHECR-2010, Nagoya]

19 TA X max distributions (I) Telescope

20 TA X max distributions (II) Telescope

21 ANISOTROPIES Telescope

22 Sky distribution, E > 10 EeV E>10 EeV Telescope Equatorial coordinates, 655 events

23 Sky distribution, E > 40 EeV Telescope Equatorial coordinates, 35 events

24 Sky distribution, E > 57 EeV Telescope Equatorial coordinates, 15 events

25 Search for clustering at small scales E > 10 EeV Telescope = no excess over background

26 Search for clustering at small scales E > 40 EeV Telescope = no excess over background

27 Test of correlations with AGN 472 AGN from 2006 Veron catalog with z < (D < 75 Mpc) separation angle 3.1 CR E>57 EeV Telescope AGN z<0.018 Equatorial coordinates

28 Test of correlations with AGN 16 N_corr expectation data background N_tot Telescope Currently: observed 6, background 3.6, p = 16% = compatible with background

29 Correlation with LSS UHECR flux at high energies is expected to be anisotropic because matter distribution is not uniform at distances 100 Mpc The matter distribution can be modeled out to 250 Mpc from the XSCz catalog (T. Jarrett, in preparation) containing over galaxies with spectroscopic redshifts From the matter distribution the UHECR flux map may be calculated and compared to observation This involves a single parameter the smearing angle θ representing deflections in magnetic fields and finite angular resolution Telescope

30 Correlations with LSS E > 40 EeV Telescope Galactic coordinates

31 Correlations with LSS E > 57 EeV Telescope Galactic coordinates

32 Results of the statistical tests probability NULL = structure E>40 EeV NULL = iso 95% CL smearing angle, degrees Compatible with both structure and isotropy Telescope

33 Results of the statistical tests probability NULL = structure NULL = iso E>57 EeV 95% CL smearing angle, degrees Compatible with structure not compatible with 95%CL Telescope

34 PHOTON LIMIT Telescope

35 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 Telescope Log E min ev G.Rubtsov, JPS March 2010; Quarks 10

36 CONCLUSIONS TA observes the cut-off in the spectrum, significance currently is 3.5σ TA data favor light at high energies (like HiRes, unlike Auger) Almost fully consistent with isotropy (except perhaps at E > 57 EeV) no significant small-scale clustering no significant correlation with AGN no significant correlation with LSS Telescope

37 BACKUP SLIDES Telescope

38 TA surface in detail < Surface Detector > GPS scintillator box wlan (2.4GHz) solarpanel (120w) WLSF: 1.0mmφ (2cm separation) PMTs: 3m 2 ET 9123SA 2 (12mm 2 layers) 200kg electronics box + battery (100Ah) Telescope

39 atmosphere monitoring < Atmospheric Monitor (LIDAR, CLF) & LINAC > back-scat. side-scat. Telescope LIDAR electron shower LINAC 40MeV 10 9 e (6.4mJ) CLF 100m 20.85km

40 SD event example Telescope

41 FD event example Telescope

42 Energy scale Telescope SD energy: CORSIKA QGSJET-II full MC FD energy: MD mono, BRM, LR hybrid Result: E = E SD /1.27

43 Statistical significance of GZK cut-off Telescope G.Thomson, ICHEP 10, Paris

44 Auger & HiRES XMAX results Auger: Phys.Rev.Lett ] 2 <X max> [g/cm QGSJET01 QGSJETII Sibyll2.1 EPOSv proton E [ev] HiRES: Phys.Rev.Lett iron ] 2 ) [g/cm max RMS(X proton iron E [ev] Telescope

45 Telescope C: Centaurus supercluster (60 Mpc); Ca: Canes I group (4 Mpc) and Canes II group (9 Mpc); Co: Coma cluster (90 Mpc); E: Eridanus cluster (30 Mpc); F: Fornax cluster (20 Mpc); He: Hercules superclusters (140 Mpc); Hy: Hydra supercluster (50 Mpc); L: Leo supercluster (130 Mpc), Leo I group (10 Mpc), and Leo II group (20 Mpc); M81: M81 group (4 Mpc); M101: M101 group (8 Mpc); P: Pegasus cluster (60 Mpc); PI: Pavo-Indus supercluster (70 Mpc); PC: Pisces- Cetus supercluster (250 Mpc); PP: Perseus-Pisces supercluster (70 Mpc); S: Shapley supercluster (200 Mpc); UM: Ursa Major supercluster (240 Mpc), Ursa Major North group (20 Mpc), and Ursa Major South group (20 Mpc); V: Virgo cluster (20 Mpc); VII: Virgo II group (20 Mpc); VIII: Virgo III group (20 Mpc).

46 The statistical test ( flux sampling ) Telescope Events following the model would produce uniform distribution over the bands No binning is needed (on the picture it is for illustration only): two distributions may be compared by the KS test