physics laboratory
DESCRIPTION
Physics Laboratory. School of Science and Technology. Hellenic Open University. Απόστολος Τσιριγώτης. Αξιολόγηση Αρχιτεκτονικών και Υποθαλάσσιων Περιοχών Εγκατάστασης για ένα Μεγάλο Μεσογειακό Τηλεσκόπιο Νετρίνων. Α. Τσιριγώτης - PowerPoint PPT PresentationTRANSCRIPT
Απόστολος Απόστολος ΤσιριγώτηςΤσιριγώτης
Αξιολόγηση Αρχιτεκτονικών και Αξιολόγηση Αρχιτεκτονικών και Υποθαλάσσιων Περιοχών Υποθαλάσσιων Περιοχών
Εγκατάστασης για ένα Μεγάλο Εγκατάστασης για ένα Μεγάλο Μεσογειακό Τηλεσκόπιο Μεσογειακό Τηλεσκόπιο
ΝετρίνωνΝετρίνωνΑ. ΤσιριγώτηςΑ. Τσιριγώτης
Β. Βεργανελάκης, Α. Λέισος, Γ. Μπουρλής,, Α. Σκόδρας , Σ. Τζαμαρίας Β. Βεργανελάκης, Α. Λέισος, Γ. Μπουρλής,, Α. Σκόδρας , Σ. Τζαμαρίας
The HOU software chain
Underwater Detector
•Generation of atmospheric muons and neutrino events (done – Techn. Note)
•Detailed detector simulation (GEANT4) (done – Techn. Note)
•Optical noise and Photomultiplier (PMT) response simulation (done)
•Filtering Algorithms (done – Techn. Note) …
•Muon reconstruction (done – Techn. Note) …
Calibration (Sea top) Detector
•Atmospheric Shower Simulation (done – Techn. Note)
•Muon and Neutrino Transportation to the Underwater Detector (done)
•Reconstruction of the shower direction (done – Techn. Note) …
•Estimation of: resolution, offset, PMT position (done – 2 draft papers in NIM )
Code will be available at http://physicslab.eap.grDocumentation in progress
Event Generation – Flux Parameterization
•Neutrino Interaction Events
•Atmospheric Muon Generation (2 Parameterization Models)
μ
Atmospheric Neutrinosν
ν
Cosmic Neutrinos
Earth
Shadowing of neutrinos by Earth
Nadir Angle
Pro
bab
ilit
y o
f a
ν μ t
o c
ross
Ear
th
GEANT4 Simulation – Detector and Physics Description
• Any detector geometry can be described in a very effective way
• All the relevant physics processes are included in the simulation
GEANT4 Simulation – Primary Particles
•Any type of secondary particle and it’s interactions is simulated
•All the interactions and transportations of the secondary particles are simulated
•For the simulation of the neutrino nucleon interaction PYTHIA is used
GEANT4 Simulation – Fast Simulation techniques
•Electromagnetic Shower Parameterization
•Simulation of optical photons continues after emission only when there is a significant probability for the photon to hit a PMT
GEANT4 Simulation : Visualization
Particle tracks, detector components and hits are visualized using Virtual Reality Modeling Language (VRML)
GEANT4 Simulation – Example: Charge Current Atmospheric νe (20GeV) interaction
Detector Geometry Optical Module Geometry
1km3 Grid with 18522 PMTs
Particle Tracks
Hits
PMT Photocathod
PMT Collective Efficiency
PMT Single Photoelectron Spectrum
mV
PMT Quantum Efficiency
PMT Standard electrical pulse for a response to a single p.e.
PMT Arrival Pulse Time resolution
Optical noise and PMT response simulation
Radioactive decays in water
Simulation Example
1km3 Grid - 1 TeV Vertically incident muon
K40 Noise Hits
Signal Hits
(Hit amplitudes > 2 photoelectrons)
Electrical Pulse of a Noise Hit
Filtering & Reconstruction Algorithms
Local (storey) Coincidence filterApplicable only when there are more than one PMT looking towards the same hemisphere
Global clustering (causality) filter50% Background rejection while all signal hits survive (1km3 Grid & 1 TeV muon)
Local clustering (causality) filter75% Background rejection while 90% of signal hits survive (1km3 Grid & 1 TeV muon)
Prefit : Clustering of candidate tracks
Angular deviation (degrees)
1TeV muons
1km3 Grid Detector
Fit:Kalman Filter (novel application in this area)
Angular deviation (degrees)
1TeV muons
1km3 Grid Detector
PRELIMINARYPRELIMINARY
The HELYCON Detector Module:
CONSTRUCTION
SC-301 Protvino
BICRON BCF91A
12 fibers/column
TYVEC 4650B
PH: XP1912
10 x 12 cm tiles
2x80 tiles ~ 0.96 m2
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
Response to ShowersData versus Monte Carlo Prediction
PRELIMINARY
deposited charge per counter [mip equivalent]
Data
___ M.C. Prediction
zenith angle (θ)
φ
Observed Rates: 2500 (± 30 ) per day
Predicted Rates: 2430 (± 100 M.C. stat.) per day
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
Measuring the angular resolution of a single station
Discriminator
(1.5 MIP)
Input C Trigger
Input B
Input A’
Input A
Input B’
Detector I: A, B,C
Detector II: A’, B’,C
~10m
between
detectors
θΙ-θΙΙ
M.C. Prediction
10m lever arm
6.8o·(2)1/2=9.6o
HELYCONHELLENIC LYCEUM COSMIC OBSERVATORIES NETWORK
1019 eV
1017 eV
1015 eV
2 km
The General Idea…
•Angular offset
•Efficiency
•Resolution
•Position
but also Physics …
C.R. composition
UHE ν - Horizontal Showers
Veto atmospheric background – Study background
We propose a minimum of 3 stations with at least 4 m2 scintillator
detectors each
Floating stations
(Sea Technology?)
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]
•KM3NeT Kick-off Meeting, 11-13 April 2006, University of Erlangen-Nuremberg, Germany (1. Simulation and Reconstruction Algorithms, 2. Event Selection Criteria and Filters and 3. Calibrating the KM3 Telescope with EAS )•HEP2006: Recent Developments in High Energy Physics and Cosmology, April 13-16 2006, Ioannina, Greece (1. Neutrino Telescopy and EAS, 2. Data Analysis Techniques for the KM3NeT and 3. Using HELYCON as a calibrating system)
•20th European Cosmic Ray Symposium, September 5th-8th 2006, Lisbon, Portugal (HELYCON Detector: A status report)
•6th International Workshop on the Identification of Dark Matter (IDM 2006), 11-16 September 2006, Rhodes Greece (Towards a SeaTop Infrastructure)
•KM3NET Physics and Simulation Meeting (WP2), 24-25 October 2006, CPPM Marseilles France (H.O.U. Analysis and Simulation Tools)
•KM3NET WP3 Meeting, 8-10 November 2006, Paris (KM3NeT: calibration with atmospheric showers)
Contributions to International Workshops and Conferences
•2nd Workshop on Cosmic Rays in Schools Projects, September 9th 2006 Lisbon Portugal (HELYCON: as an Outreach and Educational program )
Publications
•A. Tsirigotis, “HELYCON: A Status Report”, Proceedings of the 20th European Cosmic Ray Symposium
•S.E.Tzamarias, “HELYCON: towards a sea top infrastructure”, Proceedings of the 6th International Workshop on the Identification of Dark Matter
•D. Loukas et al, “HELYCON Readout Electronics”, to be published .
•A.Leisos et al, “KM3NeT: Calibration with Atmospheric Showers”, to be published (NIM)
•A.Tsirigotis et al, “The HELYCON Detector”, to be published in Astr. Phys.