experimental method experimental method kihyeon cho kyungpook national university spring semester...
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Experimental Experimental
MethodMethodKihyeon Cho
Kyungpook National University
Spring Semester 2005Spring Semester 2005Experimental Method and Data ProcessExperimental Method and Data Process
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
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 FastBUSSoftware : Dos, Windows, NT, and Linux(Unix) with C, C++, BASIC, o
r FORTRAN languages.
DAQ with VME,CAMAC and NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
Experiment setup.
DAQ with VME,CAMAC and NIMDAQ 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 ?
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
What kind of data do you take?
Count SCALOR
Charge total charge ADC charge shape SHAPER + ADC
Time TDC
DAQ with VME,CAMAC and NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
With what hardware do you take data?
VME Versa Module Eurocard
CAMAC Computer Automated MeasurementAnd Control
NIM Nuclear Instrumentation Modules
GPIB General Purpose Interface Bus
DAQ with VME,CAMAC and NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
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 NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
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 NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
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 NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
Programming at CHEP
Dos(GPIB and CAMAC)
Visual BASIC(GPIB and CAMAC)
Linux(VME controller)
DAQ with VME,CAMAC and NIMDAQ with VME,CAMAC and NIM
DAQ with VME,CAMAC and DAQ with VME,CAMAC and NIMNIM
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 NIMDAQ with VME,CAMAC and NIM
An Experimental Study ofCosmic Rays Spectrum
Using a Scintillator Detector
by D.Kim
Contents
• Introduction• Cosmic Rays• Simulation• DAQ system• Data• Conclusion & Discussion
Introduction
SimulationDetection
Flux w.r.t. distance between panels
Flux w.r.t. angle of inclination of panelof cosmic rays
Investigating the characteristics of the detector
Constructing the DAQ system
Cosmic Rays
• These “rays” were discovered by Victor Hess in 1912.
• The name “cosmic rays” were given by Millikan in 1925.
• Energy & rate– ~106eV, most cosmic ray particles– Above 1018eV, 1 / km2 / week– Above 1020eV, 1 / km2 / 100years– cf. 1012eV @FNAL
• These rays are FREE!
Primary Cosmic Rays
• Primary cosmic rays aredefined as all particles thatcome to Earth from outerspace.
Secondary Cosmic Rays• Collision of primary cosmic
rays with atoms in the upperatmosphere produce mostlyneutral and charged pions.
• Decay mode of pion, muon– 7.8045m
– 21.1m
– 658.654m
• At sea level, most of themare muons.
0
2
e e
)( c
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~
))min(/(cos),( 22 steradcmj
min))(/(2
cos),(2/
0
2
0
cmdj
Simulation)cos,sin,0( A
)cos,sinsin,cos(sin p djJ Ap),(
R: an uniform random number on [0,1]
lw
O
),( wRlR
)2,(cos),( 3/11 RR
n: number of event
hit: number of passing through both panels
Cosmic rays rate through both panels (angle, distance) ~ J x hit /n
Simulation Programx
y
z
Schematic Electronics
Gate Generator
ADC
VMEMasterModule
PCIADA
PC
OS: Linux
AND
Discriminator
Cosmic Ray
Detector 1
Detector 2
DAQ Program
Experimental ArrangementFan In Fan Out
DiscriminatorCoincidence
Gate Generator ADC
VMEMasterModule
PCIADA
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
How to Believe Cosmic Rays
H.V.=1050V
Th.=-25mV308s
Th.=-25mV249s
Th.=-25mV2417s
Th.=-25mV2430s
Th.=-100mV3462s
Th.=-120mV3956s
Detector 1 Detector 2
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.
Flux w.r.t. AngleFlux(/min)
Real data
Histogram: MC
Angle(degree)
Scintillator size: 15 cm x 19.5 cm
The distance between panels: 50cm
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.