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Search for time correlations in atmospheric muon arrival times in the ANTARES Telescope Laboratoire de Physique, Radiation et Matière LPRM, Oujda 1 CERN,

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Presentation on theme: "Search for time correlations in atmospheric muon arrival times in the ANTARES Telescope Laboratoire de Physique, Radiation et Matière LPRM, Oujda 1 CERN,"— Presentation transcript:

1 Search for time correlations in atmospheric muon arrival times in the ANTARES Telescope Laboratoire de Physique, Radiation et Matière LPRM, Oujda 1 CERN, 28 Juin 2012 Y. Tayalati, A. Moussa, A. Rrhioua & M. Hamal

2 ANTARES 2  Neutrinos de haute énergie émis par des accélérateurs cosmiques

3 ANTARES 3 900 Modules Optiques (OM) 12 lignes 25 étages/ligne 3 OM/étage

4 ANTARES 4

5 5 http://www.pi1.physik.uni-erlangen.de/antares/online-display/online- display.php

6 Recherche des corrélation temporelle It is generally assumed that galactic cosmic rays have a random arrival time. They could be some mechanisms which may introduce some modulations on this distribution. higher precision measurements did not report any effect - S.P. Ahlen et al., Nucl. Phys. B 370 (1992) 432; - C. Morello et al., Nuovo Cimento 7C (1984) 682; - N. Ochi et al., Proc. 28th ICRC 1 (2003) 195. 6

7 Astroparticle Physics 23 (2005) 341–348 MACRO The results of their analyses with high statistics confirm a random arrival time distribution of high energy cosmic rays. 7 Distribution of the time separation of single muons, Distribution of the time separation of double muons

8 - C. L. Bhat et al., Nature 288 (1980) 146. - G. Badino et al., Nuovo Cimento 28 (1980) 93 They have been studying1 the distribution of the arrival times of atmospheric Cerenkov light pulses, initiated by cosmic rays of energy ≥10^14 eV. They detected a nonrandom component for time separations <40 s, and they discussed the possibility that it has a point-source origin. 8

9 DATA - /hpss/in2p3.fr/group/antares/user/schussl/data/SeaTray/prod_2011-05/ AntDST/v1r2p3_FullAntDST - e3D_SCANa Triggers - AntDST/v1r2p4/NtuplesProd: to processe Ttrees for the time study - ana_time, ana_scan: - VO: Magrid : “ www.magrid.ma” 9

10 CutFlow - muon_ttheta <Pi/2. (only down going muons) - theAntDST.GetStrategy(thisStrategy).GetRecQuality()>-6. To improve (after a comparison with MC!). Cuts on: -Nlines, nhits, livetime, angError … 10

11 CutFlow 11

12 CutFlow 12

13 CutFlow 13

14 Time correlation analyses For each muon arriving at t_0, we study the time difference with the next five following muons : 14

15 Time correlation analyses 15 For random arrivals, the time distribution may be fitted to the Gamma function of order M For M = 1 the equation reduces to an exponential

16 Time correlation analyses 16 Distribution of the time between two consecutive muons. Medium Frequency range.

17 Time correlation analyses 17 higher order

18 18 Time correlation analyses Distribution of the time between two consecutive muons. Medium Frequency range.

19 19 Burst search new analysis on muon time series in order to find isolated clusters of events. If we consider an interval Δ ≡ [A,B] of a continuous variable x and a Poisson process with density λ. We call scan statistics (SS) the largest number of events found in any subinterval of [A,B] of length ω

20 20 Burst search The probability P that a statistical fluctuation would produce a burst of events as large as k can be approximated by Terranova F., Nucl. Instrum.Methods A, 519 (2004) 659.

21 21 Burst search Terranova F., Nucl. Instrum.Methods A, 519 (2004) 659.

22 22 Distribution of the S(w) Scan Statistic variable for the windows w =30 s; w =5 min and w =30 min Burst search(MACRO) EPL, 87 (2009) 39001

23 23 Burst search(MACRO) Scan Statistic probability distributions for the windows w =30 s; w =5 min and w =30 min

24 24 Burst search(ANTARES) Distribution of the S(w) SS variable for the windows w = 20s (left panel) and w = 60s (right panel).

25 25 Burst search(ANTARES) Scan Statistic probability distributions for the windows, used in this work, w = 20s (left panel) and w = 60s (right panel).

26 26 On NEMO results !

27 Etude des GRB. http://antares.in2p3.fr/users/bouwhuis/internal/grb_ data_archive.html GCN alert messages received by Antares DAQ 27 53 (INTEGRAL), 61, 97 and 98 (Swift), 110 (Fermi, in very rare cases packet_id 111)

28 Data 28 The normal way to process the L0_data is : 1- Decode the GCN Alert 2- Filter the data 3- Reconstruct the Data

29 29 Perspective The results of our analyses confirm with high statistics a random arrival time distribution of high energy cosmic rays. Search for bursts using the SS method show No significant deviations from the null hypothesis was found. - spectrum analyses - Analyses in narrow cones - Kolmogorov–Smirnov test

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