1. Performance of CRTNT for Sub-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 UHE τ neutrinos (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. Millard County Utah/USA ~600 Scintillators (1.2 km spacing) AGASA x 9 3 x Fluorescence Stations AGASA x 4 phase-1 TA Detector Configuration ExpRes. AGAS A 1.6 0 TA SD~1.0 0 TA FD0.6 0 TA Hyb.0.4 0 Low Energy Extension Of TA in Hybrid TALE TA

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

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

12. CRTNT Detector 2.3m 3.0m Shower imaging camera: 16x16 40mm hexagonal Photonis PMT array A half of Connex box 20 Φ 600mm spherical mirror, reflectivity 82%

13. Detector Structure Remote control door 256 pixels On board FADC electronics UV filter ~5m 2 spherical Al reflector

14. Main tower detector 12 telescopes 64º 21º35º 10m 7m7m

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

18. Detector Design: Electronics 848 pe 440 ns 160 pe 240 ns sky noise background: 40 photon/ μ sec/m 2 single channel trigger: signal/noise ratio>3.5σ 320 ns running widow 3 histories of 6 μ sec per event stored 320 ns window

19. Characteristics of pulses 1000 events: 6X10 7 GeV <E< 3X10 9 GeV Pulse Width (ns) # of pe’s per 20 ns bin LG HG

20. Status of Prototype Construction $0.3M for two prototype telescopes 512 PMT ’ s calibration by Aug., 2 modified connext boxes by June 40 Φ600mm mirrors mounted by Aug. Analog electronics by July. Single channel trigger digital board by Sept. 10 m 2 UV filter by Sept. Event trigger board & I/O by Nov.

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

24. Cerenkov/edge events

25. Aperture of CRTNT

26. Impact Parameter to the Tower Detector

27. Azimuth Angle 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 km 2 sr @ 0.1EeV 20k events per year (>0.1EeV, flat aperture) 550 events per yr (>1EeV, full aperture) for cross-calibration with TALE