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Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement

Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement. Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005. Outline. Motivation of CRTNT project Design of CRTNT Status of prototype detector construction Simulation Aperture and event rate Conclusion. Motivation.

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Performance of CRTNT for Sub-EeV Cosmoc Ray Measurement

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  1. Performance of CRTNT forSub-EeV Cosmoc Ray Measurement Zhen Cao IHEP, Beijing & Univ. of Utah, SLC Aspen, CO, 04/2005

  2. Outline • Motivation of CRTNT project • Design of CRTNT • Status of prototype detector construction • Simulation • Aperture and event rate • Conclusion

  3. Motivation • UHEτneutrinos (Z.Cao et al., J. Phys. G: 31 (2005) 571-582) • Sub-EeV Cosmic Rays

  4. UHECR Energy Spectrum Structure

  5. No Absolute Calibration

  6. Poor Measurement on Composition

  7. HiRes/MIA, HeverahPark,Cerenkov etc

  8. CR arrival direction: Anisotropy

  9. TA Millard County Utah/USA phase-1 TA Detector Configuration ~600 Scintillators (1.2 km spacing) AGASA x 9 TALE Low Energy Extension Of TA in Hybrid 3 x Fluorescence Stations AGASA x 4

  10. UHECR Research Strategyco-site, cross-calibration ,dedicate access? X CRTNT TALE TA/Auger

  11. CRTNT Detector Design& Prototype • Mobile • High sensitivity • Big dynamic range

  12. CRTNT Detector • Shower imaging camera: • 16x16 40mm hexagonal • PhotonisPMT array • A half of Connex box • 20 Φ600mm spherical • mirror, reflectivity 82% 2.3m 3.0m 2.3m

  13. Detector Structure • Remote control door • 256 pixels • On board FADC electronics • UV filter • ~5m2 spherical Al reflector

  14. Main tower detector12 telescopes 21º 35º 64º 7m 10m

  15. F/C light Detector Linux box

  16. Detector Design: Optics Spherical mirror: R=4490mm Focal plane camera: D=2305mm Hexagonal pixel size: A=40mm Mirror reflectivity: R=82% UV filter transmission: T=80% Physical optical spot: about the size of the pixel

  17. Trigger/read out Electronics FPGA: single channel trigger 3.5σ Digital adjustable HV supply 4 pole filter, x 30 Amp (H) x 3 Amp (L) 50 MHz 10 bit FADC: High gain: 3 count/pe Low gain: 0.3 count/pe

  18. Detector Design: Electronics • sky noise background: 40 photon/μsec/m2 • single channel trigger: signal/noise ratio>3.5σ • 320 ns running widow • 3 histories of 6μsec per event stored 848 pe 440 ns 160 pe 240 ns 320 ns window 320 ns window

  19. Characteristics of pulses 1000 events: 6X107GeV<E< 3X109GeV HG LG Pulse Width (ns) # of pe’s per 20 ns bin

  20. $0.3M for two prototype telescopes 512 PMT’s calibration by Aug., 2 modified connext boxes by June 40Φ600mmmirrors mounted by Aug. Analog electronics by July. Single channel trigger digital board by Sept. 10 m2 UV filter by Sept. Event trigger board & I/O by Nov. Status of Prototype Construction

  21. Simulation & Performance

  22. Simulation for CRTNT • Detector configuration (3 site stereo) • Proton primary • Corsika+QGSJet based parameterization • Single channel (tube) trigger: 3.5σ • Telescope trigger: any 6 channels • Event trigger: main tower && (one of sides) • Cuts: edge events, Cerenkov light events

  23. 8km E1,2 W1,2 3km CRTNT Configuration 1-12 • Portable fluorescence detectors • 3 site stereo (12+2+2)

  24. Cerenkov/edge events

  25. Aperture of CRTNT

  26. Impact Parameter to the Tower Detector

  27. AzimuthAngle distribution

  28. Zenith angle distribution

  29. Event distribution

  30. Event Rate

  31. Shower angular resolution

  32. Conclusion • The CRTNT is dedicated to the “second knee” • All components for prototype are ordered • Constr. /Testing in lab until the end of this year • On-site testing/calibration/background next year • Simulated aperture ~ 30 km2 sr @ 0.1EeV • 20k events per year (>0.1EeV, flat aperture) • 550 events per yr (>1EeV, full aperture) for cross-calibration with TALE

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