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![Page 1: Antonis Leisos KM3NeT Design Study the calibration principle using atmospheric showers the calibration principle using atmospheric showers construction.](https://reader035.fdocuments.in/reader035/viewer/2022062315/56649d0b5503460f949dde2a/html5/thumbnails/1.jpg)
Antonis LeisosAntonis Leisos
KM3NeT Design StudyKM3NeT Design Study
• 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
XXV Workshop on Recent Developments in High Energy Physics & Cosmology
NTUA Greece 28 - 31 March 2007
Calibration systems and methods for underwater neutrino telescopeCalibration systems and methods for underwater neutrino telescope
G. Bourlis, E. P. Christopoulou, N. Fragoulis, N. Gizani, A. Leisos, S. E. Tzamarias, A. Tsirigotis, B. Verganelakis
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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
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The General Idea…
•Angular offset
•Efficiency
•Resolution
•Position
Physics ? (ex. ICETOP)
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
We propose a minimum of 3 stations with at least 16 m2 scintillator
detectors each
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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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The HELYCON Detector Module
Scintillator 2
Scintillator 3
GPS timestamp
Station Server
Scintillator 3
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Simulation Tools
CORSIKA(Extensive Air Shower
Simulation)
GEANT4(Scintillation, WLS & PMT response)
Fast Simulation also available
Number of particles to the ground
Energy: 105 GeV – 5 105 GeV
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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
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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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Monte Carlo Studies
Reconstruction efficiency Resolution (degrees)
Three Stations Working Independently for 10 days
Single Station: 4 detectors (1m2 plastic scintillator), 20 m distance between the detectors, three out of four selection trigger
PRELIMINARY
Minimum of total collected charge [mip equivalent]zen
ith
an
gle
re
so
luti
on
[d
eg
ree
s]
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dt=0
Proposed Detector
19m
19m
5m
1 m2 Scintillation Counter
dt1
dt2
dt3
2
exp2 i
hits dt
dt dt
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curvature
thickness
Tim
e S
pre
ad
(n
s)
Multi-Station Operation Monte Carlo Studies in Progress
Total collected charge [pe]
First coming particles
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Timing vs Pulse Hight
Input A
Input B
Discriminator
(1.5 MIP)
Trigger
Slewing
Resolution
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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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Consistent Estimations
g g ˆ ˆ( , ) ( , )R 2 2χ χ
Tg g
1
g g
ˆ ˆ-Λ = D
ˆ ˆ- -
2 (P R,2) 2 (P ,2)
Minuit Minimization
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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 Propagation
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)
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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)
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Effective Area
log(E) (GeV)
2Effective Area (m )
~ 30 showers per day reconstructed at the surface and in the deep sea
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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…