1. Lulin Background Measurement and Detector Issues NuTel project NTU, Taiwan Во время этого доклада может возникнуть дискуссия с предложениями конкретных действий. Используйте PowerPoint для записи предложений по ходу обсуждения: Во время демонстрации щелкните правой кнопкой мыши Выберите Записная книжка Выберите вкладку Действия Вводите замечания по мере поступления Нажмите кнопку ОК по завершении доклада В результате в конец презентации автоматически будет добавлен слайд Действия со списком внесенных предложений. K.Ueno

2. Outline  Schedule of 2002  Design of detector/electronics  LuLin test  Calibration  Detector thought  Conclusion

3. Schedule of 2002  May – July: design and fabrication of electronics, detector and software. Most was made from scratch.  August – September: debugging full telescope system.  October: LuLin observatory test in moonless nights.  October – December: data analysis and calibration.

4. Design of detector/electronics  Main task of this design – create a simple equipment for the measurement of background light from a mountain.

5. Preamplifier schematics + - From PMT + - From PMT First version (current -> voltage) Second version (charge -> voltage) Gain~100mV/1p.e RC=500ns Power supply (16-channels preamplifier): 380mA on +/- 5V (3.8W, 240mW/channel)

6. Preamplifier test with test pulse Q~3*10^7 e (~10 photons)

7. Hamamatsu PMT test Uniformity from different channels Measured at NTUData from Hamamatsu Broken PMT

8. Design of detector/electronics  Receiver parameters: Gain: 1 (~100mV/pe) Noise: ~5mV rms There is a small problem: an overshoot in the tail. + - Shaper Comparator LVDS transmitter To Trigger From preamp. 100 nS Delay line To ADC

9. Design of detector/electronics  Trigger: using our TTM2 module made for BELLE experiment (in VME + FPGA based) changing firmware code – one week only! Use this LVDS-level connector

10. Design of detector/electronics  Trigger: from TTM2 to NuTel Trigger Change 3 IC (transmitters onto receivers)

11. Design of detector/electronics  ADC – use industrial one (Acromag ADC): Inputs: differential 32 channels for simultaneous conversion Dead time: ~10  s (8  s – from data sheet!) Operation clock: 8MHz (there is a jitter 125ns) Range: +/- 10V (14 bit, 1.25 mV/bin) Noise: ~1mV (from data sheet)  Problem: a real dead time is a bit larger than from data sheet, so we have low ADC readout rate (most time DAQ resets ADC module due problems in ADC) in case of big event rate (large photon flux), so a most information is from Trigger's counter, which operates with 60MHz clock)

12. Design of detector/electronics  DAQ: use VME connected with PC via SBS system Code: Visual C++, Windows ADC SBSPC Windows, Visual C++ ADC data On line trigger BufferRAM Hard disc Histograms Hard disc Trigger data Trigger VME

13. Design of detector/electronics  DAQ: some print-screens from software

14. Design of detector/electronics  Main task of this design – create a simple equipment for the measurement of background light from a mountain

15. LuLin test  Some pictures from LuLin observatory

16. LuLin test  Some pictures from LuLin observatory

17. LuLin test  Some pictures from night shifts

18. Sirius seen by prototype at Lulin  Study: Effective field of view Lens transmittance as function of off- axis angle.  In the future, Calibrate the pointing accuracy Monitoring telescope health

19. Lulin Set-up Lens: 15cm radius Total PMT area 1.75cm x 1.75 cm Neutral density BG3 PMT Plate Focal length 30 cm

20. How to calculate the photon flux  R    *[T2  Q(  d   photon flux [ s –1 cm -2 sr -1] A : lens area (15cm * 15 cm * 3.14)  solid angle span by total PMTs (1.75cm/30cm)^2  Neutral density factor   lens transmittance T2: BG3 transmittance (optional) Q : PMT quantum efficiency R: trigger rate

21. Transmittance of BG3, PMT, and Lens

22. Trigger-rate in different experiments

23. Photon flux in different experiments

24. Summary table Trigger – rate (mean) +- RMS (K) Photon-flux [K cm – 2, sr-1 s-1] 3deg+BG3 33.72+- 2.31 11892.64 3deg 87.332+- 3.94 13850.17 7deg +BG3 97.706+-1.93 34459.74 7deg 237.6+-3.13 37681.51 15deg+BG3 209+-14.9 73711.82 15deg 980+-17.23 155420.4 Before Sirius 364+-6.74 128378.5 Sirius 1937+-3.091 683156.9 After Sirius 274.9+-38.9 96953.96 All Sirius data are BG3 included

25. From LuLin test to Calibration  Setting thresholds on LuLin: Minimal threshold when noise data (pedestal) are never read from ADC + ~ 1 rotation of variable resistor (~ 50 mV) Thresholds during calibration: same as on LuLin  Dark current rate from 16 channels: ~ 10-20 Hz after keeping more then one hour at black box ~ 100 - 200 Hz on LuLin and at black box after operating with LED light

26. Calibration  Electronics test with test pulse: Sensitivity: ~100mV/3.3*10^6 e (1 photoelectron) ADC data with optimized timing. A most noise is due jitter in ADC ADC data with non- optimized timing. Strobe to ADC is delayed on 100 nS from optional timing

27. Calibration  Electronics test with test pulse: Cross-talk due electronics: very small We observed a change in pedestals in some channels ~0.3 mV when a signal on neighboring one is ~1.5 V (0.02% !!! cross-talk)

28. Calibration  Electronics test with pulse to LED + fiber + PMT: Cross-talk due PMT: ~1% (from data sheet) Cross-talk ~ 0.6% Cross-talk ~ 0.2%

29. Pedestals varies from channel to channel in range from –10mV to +4mV Calibration Typical pedestal distribution A noise (r.m.s.) of pedestal distribution varies from 0.6 mV (minimum) to 2.5 mV (maximum).

30. PedestalDark currentLightLimit (overflow) Calibration Test using LED pulse 100 ns x 1kHz: – Typical histogram in case of big photon flux

31. Preamp  Current amp. or charge amp.?  If charge amp., should have a small time constant to avoid a dead time.  Large dynamic range of energy is needed.  10**14~10**18 eV and a light amount depends on a detector-shower distance.  Multi-gain or logarithmic gain or both?  Space per channel for 8X8 MAPMT is already tight.

32. Timing measurement  Need to cover a large coincidence time window of 1 us or more  a pipeline DAQ.  What clock rate? Normally 40 MHz.  If we can assume a simple and uniform shape, the time resolution can be much smaller than the clock period in offline.  If a pulse shape is complex and not simple depending on a direct Cerenkov or a fluorescence, the rate should be higher.

33. Trigger  A simple coincidence among detectors may have too many fake triggers.  Time info. must be associated w. the pixel angular info. to reduce the fakes.  The association can be best done in hardware. Possible?  If not, must be done in a higher-level software trigger. Longer time to decide.

34. T T Det1 Det2 θ Shower Det1 Det2 Δt 12 A candidate combination of Det1 & 2 signals is searched for in a time window. A trigger accepts a correct combination of  t and .

35. Monitor and control  Ideally a physics event or constant should be used as a monitor. But looks difficult.  Environmental parameters such as temperatures etc. must be monitored.  HV/LV monitor and remote control.

36. Alignment and calibration  Reflected lights of a laser beam can simulate EAS and can be used for alignment.  Need a GPS system for a detector position and a time stamp.  Need a good scheme to synchronize sub- detectors over a long distance.  Is there a ‘gold-plated’ event available for alignment and calibration?

37. Need to worry many more MDAQ SDAQ Optics SDAQ Optics SDAQ Optics PMT/PAWire/Wireless How to get power. Make SDAQ low-power. SDAQ-MDAQ communication. MAPMT maintenance. Hostile environment. etc. ………..

38. Conclusion  A telescope (a detector and its electronics) were made in a short time to gain some experience.  Clear signals for a background and Sirius were observed, for demonstration, at Lulin observatory in October moonless nights.  A BG trigger rate was 130 photons/m**2 sr ns at 1 p.e. threshold.  Calibration is still under way.  A new design of a telescope will be made based on the experience.