1. Experimental Method Experimental Method Kihyeon Cho Kyungpook National University Spring Semester 2005 Experimental Method and Data Process

2. What will you do?  What kind of data do you take? Cosmic ray ’ s count, Energy, momentum, charge etc. Particle ’ s count, identification, and characteristic. With total charge, signal shape, or time information.  How do you take data? Hardware : VME, CAMAC, NIM, GPIB, and FastBUS Software : Dos, Windows, NT, and Linux(Unix) with C, C++, BASIC, or FORTRAN languages. DAQ with VME,CAMAC and NIM

3.  Experiment setup. DAQ with VME,CAMAC and NIM What kind of data do you take? With what hardware do you take data ? With what software do you take data ?

4. What kind of data do you take?  Count  SCALOR  Charge  total charge  ADC  charge shape  SHAPER + ADC  Time  TDC DAQ with VME,CAMAC and NIM

5. With what hardware do you take data?  VME  Versa Module Eurocard  CAMAC  Computer Automated Measurement And Control  NIM  Nuclear Instrumentation Modules  GPIB  General Purpose Interface Bus DAQ with VME,CAMAC and NIM

6. With what software do you take data?  Operating System  Driver dependent.  C,C++  Dos, Windows, and Linux(Unix)  Visual Basic,Visual C++  GUI, user friendly.  q-Basic, Fortran  Linux, Windows DAQ with VME,CAMAC and NIM

7.  NIM modules Fan-in Fan-out  to make several same analog signal Amplifier  to amplify analog input signal Discriminator  to change analog to digital pulse w.r.t threshold Gate generator  gate generating module Scaler  to count input signal AND or OR unit  to calculate logical signal DAQ with VME,CAMAC and NIM

8.  VME or CAMAC modules(computer based modules) ADC  Analog to Digital converter TDC  Time to Digital converter Gate generator  gate generating module Scaler  to count input signal GPIB to CAMAC interface  to take data from CAMAC modules VMEMM interface  to take data from VME modules. Amplifier  to amplify analog input signal Discriminator  to change analog to digital pulse w.r.t threshold DAQ with VME,CAMAC and NIM

9.  Programming at CHEP  Dos(GPIB and CAMAC)  Visual BASIC(GPIB and CAMAC)  Linux(VME controller) DAQ with VME,CAMAC and NIM

10.  Linux with VME controller  PCIADA and VMEMM card  Linux driver install  PCIADA and VMEMM Card check.  Hardware setup  Programming with C or C++ with ROOT library. DAQ with VME,CAMAC and NIM

11. An Experimental Study of Cosmic Rays Spectrum Using a Scintillator Detector by D.Kim

12. Contents Introduction Cosmic Rays Simulation DAQ system Data Conclusion & Discussion

13. Introduction SimulationDetection Flux w.r.t. distance between panels Flux w.r.t. angle of inclination of panel of cosmic rays Investigating the characteristics of the detector Constructing the DAQ system

14. Cosmic Rays These “ rays ” were discovered by Victor Hess in 1912. The name “ cosmic rays ” were given by Millikan in 1925. Energy & rate –~10 6 eV, most cosmic ray particles –Above 10 18 eV, 1 / km 2 / week –Above 10 20 eV, 1 / km 2 / 100years –cf. 10 12 eV @FNAL These rays are FREE!

15. Primary Cosmic Rays Primary cosmic rays are defined as all particles that come to Earth from outer space.

16. Secondary Cosmic Rays Collision of primary cosmic rays with atoms in the upper atmosphere produce mostly neutral and charged pions. Decay mode of pion, muon –7.8045m –21.1m –658.654m At sea level, most of them are muons.

17. Cosmic Ray Flux The flux of cosmic rays is –The relativistic boost in the primary direction is much greater than at angle to the vertical. –The longer they travel through the atmosphere, the more energy they lose to ionization, and the more likely they are to decay before reaching the detector Total rate of cosmic rays~

18. Simulation R: an uniform random number on [0,1] l w O n: number of event hit: number of passing through both panels Cosmic rays rate through both panels (angle, distance) ~ J x hit /n Simulation Program x y z

19. Schematic Electronics Gate Generator ADC VMEMasterModule PCIADA PC OS: Linux AND Discriminator Cosmic Ray Detector 1 Detector 2 DAQ Program

20. Experimental Arrangement Fan In Fan Out Discriminator Coincidence Gate Generator ADC VMEMasterModule PCIADA

21. Hardware Linear Fan-In/Fan-Out, LeCroy, 428F Octal Discriminator, LeCroy, 628B –threshold=-100mV,-120mV, width=120ns Quad Coincidence, LeCroy, 622 Dual Gate Generator, LeCroy, 222 –full scale width=1 us 32 Channel Multievent Charge ADC, CAEN, V792 VME Master Module, wiener PCIADA, wiener Scintillator, BC408, SAINT-GOBAIN Photomultiplier Tube, R980, SAINT-GOBAIN

22. How to Believe Cosmic Rays H.V.=1050V Th.=-25mV 308s Th.=-25mV 249s Th.=-25mV 2417s Th.=-25mV 2430s Th.=-100mV 3462s Th.=-120mV 3956s Detector 1 Detector 2

23. Flux w.r.t. Distance Flux(/min) Distance(cm) Real data Histogram: MC Scintillator size: 15 cm x 19.5 cm The normal to panel is vertical.

24. Flux w.r.t. Angle Flux(/min) Real data Histogram: MC Angle(degree) Scintillator size: 15 cm x 19.5 cm The distance between panels: 50cm

25. Conclusion & Discussion Real data is similar to the result of simulation of cosmic rays spectrum of distance between panels and angle. Programming the data acquisition, which display the ADC channel-count plot using ROOT in real time, for Linux. Needing to improve the apparatus, to identify the kind of cosmic rays. Needing to measure the energy spectrum of cosmic rays.