Physics Laboratory
description
Transcript of Physics Laboratory
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Antonis LeisosAntonis Leisos
A sea top infrastructure for A sea top infrastructure for calibrating an underwater calibrating an underwater
neutrino telescopeneutrino telescope
• the calibration principle using atmospheric showersthe calibration principle using atmospheric showers
• construction and performance of the prototype detector stationconstruction and performance of the prototype detector station
• Monte Carlo Studies Monte Carlo Studies
TeV Particle Astrophysics 2007
27-31 August 2007 Venice, Italy
G. Bourlis, P. Christopoulou, N. A. B. Gizani, A. Leisos, P. Razis ,A. G. Tsirigotis and S.E. Tzamarias
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1 km
2 km
SPASE air shower arrays
calibration of AMANDA angular resolution and pointing !
resolution Amanda-B10 ~ 3.5°
spase-amanda
IceCube IceTop
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The General Idea…
•Angular offset
•Efficiency
•Resolution
•Position
Physics ?
C.R. composition
UHE ν - Horizontal Showers
Veto atmospheric background – Study background
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~4km
~20km
Isotropic on the top of the atmosphere
BUT …
~ coscos
dN
d
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Pierre Auger: M. Are et al. Ast.Part. 14: 109-120 2000
0 23 4km instrumented area
17
0 2
for detection Ε 6×10 eV
θ 80 0.35/km /year 1.4showers/year
Haverah Park (www.ast.leeds.ac.uk/haverah/havpark.html):
12km2 effective area and 2π coverage in φ
for 10 years operation less than 100 detected showers with 0θ 80
reweightingBlind fit
Okada model NESTOR: muon flux @ 4000m
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Floating stations
The Concept
3 stations with at 16 m2 scintillator detectors each
•Angular offset
•Efficiency
•Resolution
•Position
reweightingBlind fit
Okada model
~ coscos
dN
d
NESTOR: muon flux @ 4000m
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HELYCON Station
GPSScintillator-PMT
Scintillator-PMT
Scintillator-PMT
DAQ
~20 m
1 m2
Single Station Set-Up
Triangulation
Shower Direction
Scintillator-PMT
4·(1W/counter)+30W(PC+electronics)
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Simulation Tools
CORSIKA(Extensive Air Shower
Simulation)
GEANT4(Scintillation, WLS & PMT response)
Fast Simulation also available
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Simulation Tools
DAQSIM(DAQ Simulation)
HOUANA(Analysis &
Track Reconstruction)
Time (ns)
Height (mV)
Zentih (degrees)
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Simulation Tools
GEANT4Muon Propagation to KM3
HOU-KM3Muon track (s) reconstruction
dm
L-dm
(Vx,Vy,Vz) pseudo-vertex
dγ
d
Track Parameters
θ : zenith angle φ: azimuth angle (Vx,Vy,Vz): pseudo-vertex coordinates
θc
(x,y,z)
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Monte Carlo Studies- Outlook 1014 - 5·1015 eV
E~ 1014 - 5·1015 eV: 2500 showers/m2/year
Single station detection: 351m2 effective area (depends on geometry and selection cuts)
Multi-Station: separation <100m, better resolution
E> 1016 eV: 1 shower/m2/year
TO BE STUDIED
35% of the detected showers include a muon which arrives at the Neutrino Telescope (depth 4000m) with an energy >300GeV
General Remark: 3 stations operating for 10 days can identify an angular offset with an accuracy of 0.15o
Specifically…Specifically…
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Monte Carlo Studies
Depends on:
Detector separation
Selection criteria
Shower direction
Typical Values
1) No cut: σ= 4.5ο
2) Total Collected Charge > 10 mips: σ=2.22ο
3) Total Collected Charge > 25 mips: σ=1.33ο
4) Total Collected Charge > 30 mips: σ=1.2ο
Atmospheric shower simulation by CORSIKA - muon transportation to the detector DEPTH by GEANT4 - Sea-Top Detector detailed simulation GEANT4_HOU
PRELIMINARY
Θrec-Θtrue
Angular Resolution inSingle Shower Reconstruction
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Multi Station Set upimprove resolution – higher energies
GPS Synchronisation
Δt <±6ns using sawtooth correction
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curvature
thickness
Total collected charge [pe]
Tim
e D
ela
y (
ns
)T
ime
Sp
rea
d (
ns
)
Multi-Station Operation Monte Carlo Studies in Progress
Total collected charge [pe]
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The HELYCON Detector Module
Scintillator 2
Scintillator 3
GPS timestamp
Station Server
Scintillator 3
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HELYCON ReadOut Electronics
GPS Input
USB PortTrigger Ouput4 PMT Signal Inputs
25ps accuracy TDC
HPTDC
• 32 channels (LR) – 8 Channels (HR)
•25ps (HR) to 800 ps (LR) accuracy
•Self Calibrating
D. Loucas INP DEMOKRITOS
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Response to Showers
Discriminator
(1.5 MIP)
Trigger
Input A
Input B
~10m
trigger arrival time
~60 mip’s
~50 mip’s
14.2ns
5.4ns
θ=31ο ± 8ο
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Response to Minimum Ionizing Particles
Scintillator A
Scintillator B
Lead
DAQ based on TDS5052 Tektronix (5 Gsamples/s)
discriminators
Inputs
Trigger
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Response to a MIP
DAQ S/W based on LabView
On-Line analysis - distributions
Charge (in units of mean p.e. charge)
At the Detector Center
Data
- Monte Carlo Prediction
Detailed Monte Carlo description
PRELIMINARY
Digitized Waveforms saved on hard disk
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Response to a MIP
Detector Uniformity (the worst case)
Charge (in units of mean p.e. charge)
X Y
Typical Mean Numb. of p.e. per m.i.p. : 23 (± 16% variation)
PRELIMINARY
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Response to a MIP
Detector Uniformity - Timing
Scintillator A
Scintillator B
Lead
discriminators
Inputs
Trigger
ΔΤ consistent with the difference of optical path (fiber refractive index n=1.6)
PRELIMINARY
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Timing vs Pulse Hight
thickness
Input A
Input B
Discriminator
(1.5 MIP)
Trigger
Slewing
Resolution
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Response to Showers
Trigger Detectors >1 mip
Detectors A.and.B > 0.5 mip’s
~ coscos
8.5 0.4
dN
d
zenith angle [degrees] zenith angle [degrees]
~ coscos
9.4 0.6
dN
d
Trigger Detectors > 1 mip
Detectors A.and.B > 1.5 mip’s
α=9.4±0.2
PRELIMINARY PRELIMINARY
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Lab Measurements (a)
Discriminator
(1.5 MIP)Input C Trigger
A1
A2
A3
B1
B2
B3θΑ-θΒ
μ=-0.1±0.3
σ=7.6 ± 0.2
Pull
• Deposited Charge per counter > 4 mips 6 Active counters
μ=-0.06±0.05
σ=1.02 ± 0.03
MC -Data Data
___ M.C. Prediction
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Lab Measurements (b)
Discriminator
(1.5 MIP)Input C Trigger
A1
A2
A3
B1
B2
B3
• Deposited Charge per counter > 4 mips 6 Active counters
μ=0.1±0.6
σ=4.5 ± 0.5
θm-θtr
Pull
μ=0.01±0.1
σ=0.9 ± 0.1
MC PredictionGROUP A
GROUP Bμ=0.3±0.8
σ=5.2 ± 0.8
θm-θtr
Pull
μ=0.02±0.1
σ=0.9 ± 0.1
DATA
δθ=4.6
DATA
δθ=5.6
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dt=0
16m2 Scintillator Station
19m
19m
5m
1 m2 Scintillation Counter
dt1
dt2
dt3
2
exp2 i
hits dt
dt dt
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Time corrections
deposited charge (mip)
delay (ns)
delay spread (ns)
deposited charge (mip)
Time residual
Time Residual meas true
dt
dt dt
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Detection Efficiency
Distance from Shower Impact (meters)
Distance from Shower Impact (meters)
Efficiency
Events
Number of Active Counters (trigger)
A hit is considered when there is more than 4 mips deposited charge
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Muon Propagation
μ track
km3
Geant Simulation
(propagation & Energy Loss)
Accepted if muon with E>2TeV goes through
km3
Muon Track Reconstruction
(A. Tsirigotis talk)
Zenith angle < 13 deg
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Muon vs Shower Axis
muon primaryθ - θ (deg) μ-shower Space angle (deg)
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Primary Zenith Angle Resolution
reconstructed true
Θ
θ - θ
σreconstructed trueθ - θ (deg)
• Deposited Charge per counter > 4 mips
• Number of Hits > 10
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Primary Azimuth and Space angle Resolution
reconstructed trueφ - φ (deg) Space angle (deg)
• Deposited Charge per counter > 4 mips Number of Hits > 10
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Performance Plots
Minimum number of Active counters
Minimum number of Active countersMinimum number of Active counters
2Effective Area (m )
θ resolution (deg)
Telescope Offset Resoltuion (deg)
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Charge
Time (ns)Charge (in units of mean p.e. charge)
At the Detector Center
Data
- Monte Carlo Prediction
Scintillator A
Scintillator B
Lead
discriminators
Inputs
Trigger
Data
___ M.C. Prediction
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Charge parameterization
Distance from shower core (m) Distance from shower core (m)
2Mean density (mip/m )2RMS density (mips/m )
2
( ) 1 11000
a h a
M M
r r rr C
R R
AGASA parameterization (S. Yoshida et al., J Phys. G: Nucl. Part. Phys. 20,651 (1994)
Parameters depend on
(θ, Ε, primary)
“Mean particle density registered by an active
counter”
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Primary Impact determination
total charge collected (mip)
Impact Resolution (m)
Impact x (m)
Absolute Position resolution ~ 0.5 m
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Performance Plots
Minimum number of Active counters
Minimum number of Active countersMinimum number of Active counters
2Effective Area (m )
Spatial Resolution (m)
Telescope Offset Resoltuion (deg)
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Telescope Resolution
Telescope resolution ~ 0.1 deg
Surface Area resolution ~ 1 deg
Telescope’s resolution measurement Impossible
Inter calibration
σ=0.014
σ=0.094
σ=0.062
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Conclusions
The operation of 3 stations (16 counters) for 10 days will provide:
• The determination of a possible offset with an accuracy ~ 0.05 deg
• The determination of the absolute position with an accuracy ~ 0.6 m
• Efficiency vs Energy and Zenith angle…• Resolution No!