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Hybrid Extensive Air Shower Detector Array at the University of Puebla to Study Cosmic Rays

Hybrid Extensive Air Shower Detector Array at the University of Puebla to Study Cosmic Rays. O. MARTINEZ, H. SALAZAR, L. VILLASEÑOR * + Grupo de Estudiantes Facultad de Físico-Matemáticas, Benemérita Universidad Autónoma de Puebla, Apartado Postal 1364, Puebla , Pue., 72000, México

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Hybrid Extensive Air Shower Detector Array at the University of Puebla to Study Cosmic Rays

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  1. Hybrid Extensive Air Shower Detector Array at the University of Puebla to Study Cosmic Rays O. MARTINEZ, H. SALAZAR, L. VILLASEÑOR* + Grupo de Estudiantes Facultad de Físico-Matemáticas, Benemérita Universidad Autónoma de Puebla, Apartado Postal 1364, Puebla, Pue., 72000, México *On leave of absence from Institute of Physics and Mathematics, University of Michoacan, Morelia, Mich., 58040, México EMA 05 Morelia July 18-22, 2005

  2. PMT Electron tubes 9353 K EAS Array • Area: 4000 m^2 • 10 Liquid Ssintillator Detectors (Bicron BC-517H) • 4 Water Cherenkov Detectors PMT EMI 9030 A

  3. 2200m a.s.l., 800 g/cm2. Located at Campus Universidad Autonoma de Puebla • Hybrid: Liquid Scintillator Detectors and water Cherenkov Detectors • Energy range 10^14- 10^16 eV

  4. Trigger: Coincidence of 4 central detectors (40mx40m) NIM y CAMAC. DAQ System • Uso digital Osciloscopes as ADCs. • Rate: 80 eventos/h

  5. Use CAMAC scalers to measure rates of single partícles on each detector. Day-night variations <10% Monitoring s/mean around 3%

  6. Calibration

  7. ~74 pe

  8. LabView based DAS

  9. MPV of EM peak = 0.12 VEM i.e. around 29 MeV, i.e., dominated By knock-on + decay electrons

  10. Stopping muon at 0.1 VEM Decay electron at 0.17 VEM = 41 MeV Crossing muon at 1 VEM Alarcón M. et al., NIM A 420 [1-2], 39-47 (1999).

  11. Arrival direction sinq sinf = d/c(t2-t1) Data Analysis

  12. Angular distribution inferred directly from the relative arrival times of shower front in good agreement with the literature: cosp sen 

  13. Lateral Distribution Functions Data Analysis The shower core is located as the center of gravity. • Energy Determination EAS-TOP, Astrop. Phys, 10(1999)1-9

  14. Ne, obtained for vertical showers. The fitted curve is Ik (Ne/Nek)-g, gives g=2.44±0.13 which corresponds to a spectral index of the enerfy distributions of g=2.6

  15. Muon/EM Separation Muons deposit 240 MeV in 1.20m high water and only 26 MeV in 13 cm high liquid, while electrons deposit all of their energy i.e., around 10 MeV. Therefore for 10 Mev electrons we expect: Mu/EM=24 for Cherenkov Mu/EM=2.6 for Liq. Scint. Cherenkov Liquid Scint

  16. Mass CompositionHybrid Array Solution:

  17. Iterations Start with Ne=82,300 Nmu = 32700 E0 = 233 TeV Iterations End with Ne=68000 Nmu = 18200 E0 = 196 TeV

  18. Mass CompositionNon-Hybrid Array Do a three parameter fit to :

  19. Two Identical types of Cherenkov Detectors one filled with 1.20 m of water and the other with 0.60 m, i.e., VEMC’=0.5VEMC Mass CompositionNon-Hybrid but Composite Array i.e., do independent fits of rEM and rmuon to NKG and Greissen LDF, respectively, where:

  20. Conclusions We have checked the stability and performed the calibration of the detectors. We have measured and analyzed the arrival direction of showers. We determine the energy of the primary by measuring the total number of charged particles obtaining by integration of the fitted LDF. Study of Muon/Electromagnetic ratio is underway:

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