Performance studies for the KM3NeT neutrino telescope [Elektronische Ressource] / vorgelegt von Claudio Kopper

Claudio Kopper, Physikalisches Institut 1, Universität Erlangen-Nürnberg, [e-mail]

Sujets

• Physik

Informations

• Publié par: friedrich-alexander-universitat_erlangen-nurnberg
• Publié le: 01 janvier 2010
• Nombre de lectures: 18
• Langue: English
• Poids de l'ouvrage: 6 Mo

Extrait

Performance Studies for the
KM3NeT Neutrino Telescope
Der Naturwissenschaftlichen Fakultat
der Friedrich-Alexander-Universitat Erlangen-Nurnberg
zur Erlangung des Doktorgrades
vorgelegt von
Claudio Kopper
aus ErlangenAls Dissertation genehmigt von der Naturwissenschaftlichen Fakultat
der Friedrich-Alexander-Universitat Erlangen-Nurnberg
Tag der mundlichen Prufung: 12. Marz 2010
Vorsitzender der Promotionskommission: Prof. Dr. Eberhard Bansch
Erstberichterstatter: Prof. Dr. Ulrich Katz
Zweitberichterstatter: Prof. Dr. Christian StegmannMeinen ElternContents
Introduction 9
I Basics 13
1 High energy cosmic neutrinos 15
1.1 Neutrinos in the Standard Model . . . . . . . . . . . . . . . . . . . . 15
1.2 Cosmic accelerators . . . . . . . . . . . . . . . . . . . . . . . . . . . . 16
1.2.1 The cosmic ray spectrum . . . . . . . . . . . . . . . . . . . . 16
1.2.2 Particle acceleration . . . . . . . . . . . . . . . . . . . . . . . 17
1.2.3 Neutrino production . . . . . . . . . . . . . . . . . . . . . . . 20
1.2.4 Source candidates . . . . . . . . . . . . . . . . . . . . . . . . 21
2 Neutrino telescopes 25
2.1 Detection mechanism . . . . . . . . . . . . . . . . . . . . . . . . . . . 25
2.1.1 Neutrino interaction . . . . . . . . . . . . . . . . . . . . . . . 25
2.1.2 Cherenkov radiation from charged particles . . . . . . . . . . 29
2.1.3 Muon propagation . . . . . . . . . . . . . . . . . . . . . . . . 29
2.1.4 Electromagnetic and hadronic cascades . . . . . . . . . . . . 30
2.1.5 Light propagation . . . . . . . . . . . . . . . . . . . . . . . . 31
2.1.6 Light detection . . . . . . . . . . . . . . . . . . . . . . . . . . 32
2.1.7 Triggering . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 33
2.1.8 Muon track reconstruction . . . . . . . . . . . . . . . . . . . . 33
2.1.9 Background . . . . . . . . . . . . . . . . . . . . . . . . . . . . 34
2.2 Existing neutrino telescopes . . . . . . . . . . . . . . . . . . . . . . . 38
2.2.1 Baikal . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38
2.2.2 IceCube . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 39
2.2.3 ANTARES . . . . . . . . . . . . . . . . . . . . . . . . . . . . 40
2.3 The KM3NeT project . . . . . . . . . . . . . . . . . . . . . . . . . . 42
2.3.1 Overview . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 42
2.3.2 Design possibilities . . . . . . . . . . . . . . . . . . . . . . . . 42
2.3.3 Detector sites . . . . . . . . . . . . . . . . . . . . . . . . . . . 44
5Contents
II Methodology 45
3 Software simulation and reconstruction tools 47
3.1 Legacy software tools from ANTARES . . . . . . . . . . . . . . . . . 47
3.2 Software frameworks . . . . . . . . . . . . . . . . . . . . . . . . . . . 50
3.2.1 The concept of a software framework . . . . . . . . . . . . . . 50
3.2.2 The IceTray framework . . . . . . . . . . . . . . . . . . . . . 52
3.2.3 Simulation and analysis tools for KM3NeT within the IceTray
framework - \SeaTray" . . . . . . . . . . . . . . . . . . . . . . 52
4 A new KM3NeT simulation and reconstruction chain 55
4.1 Overview and Incentive . . . . . . . . . . . . . . . . . . . . . . . . . 55
4.2 Simulation of neutrino interactions using ANIS . . . . . . . . . . . . 55
4.2.1 Event weights . . . . . . . . . . . . . . . . . . . . . . . . . . . 57
4.3 Simulation of atmospheric muons with CORSIKA . . . . . . . . . . 58
4.4 Propagation of muons to the detection volume . . . . . . . . . . . . 59
4.4.1 Modi cations for KM3NeT . . . . . . . . . . . . . . . . . . . 59
4.5 Muon propagation and Cherenkov light generation . . . . . . . . . . 59
4.5.1 Detailed simulation . . . . . . . . . . . . . . . . . . . . . . . . 60
4.5.2 Speedup of the Cherenkov light tracking algorithm for unscat-
tered light . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 63
4.6 Fast cascade light generation and propagation . . . . . . . . . . . . . 63
4.6.1 Angular light distribution . . . . . . . . . . . . . . . . . . . . 63
4.6.2 Total photon yield . . . . . . . . . . . . . . . . . . . . . . . . 65
4.6.3 Scattering table generation . . . . . . . . . . . . . . . . . . . 65
4.6.4 Light generation at optical modules . . . . . . . . . . . . . . 68
4.6.5 Optimisation for unscattered photons . . . . . . . . . . . . . 71
4.6.6 Longitudinal light distribution . . . . . . . . . . . . . . . . . 71
4.7 Adaptation of the cascade simulation approach to muons . . . . . . 73
4.7.1 Spatial segmentation . . . . . . . . . . . . . . . . . . . . . . . 74
4.7.2 Table generation . . . . . . . . . . . . . . . . . . . . . . . . . 74
4.7.3 Light generation at optical modules . . . . . . . . . . . . . . 76
4.8 A uni ed cascade/muon simulation . . . . . . . . . . . . . . . . . . . 76
4.9 Simulation of light near and in optical modules . . . . . . . . . . . . 77
4.9.1 ANTARES-style modules . . . . . . . . . . . . . . . . . . . . 77
4.9.2 MultiPMT modules . . . . . . . . . . . . . . . . . . . . . . . 79
4.10 Light detection . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 83
4.10.1 PMT simulation . . . . . . . . . . . . . . . . . . . . . . . . . 83
4.10.2 Readout electronics simulation using the \ARS" chip . . . . . 84
4.10.3 A time-over-threshold approach . . . . . . . . . . . . . . . . . 84
4.10.4 Hit coincidence triggering . . . . . . . . . . . . . . . . . . . . 85
6Contents
4.11 Muon track reconstruction strategies . . . . . . . . . . . . . . . . . . 86
4.11.1 The standard ANTARES reconstruction strategy . . . . . . . 86
4.11.2 A new reconstruction algorithm for multiPMT detectors . . . 87
5 Analysis techniques 97
5.1 Angular resolution . . . . . . . . . . . . . . . . . . . . . . . . . . . . 97
5.2 Neutrino e ective area . . . . . . . . . . . . . . . . . . . . . . . . . . 97
5.3 Point-source sensitivity and discovery potential . . . . . . . . . . . . 99
5.3.1 Discovery potential . . . . . . . . . . . . . . . . . . . . . . . . 99
5.3.2 Sensitivity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 100
III Results 103
6 Comparison between simulation chains 105
6.1 Detector design, environment and simulation parameters . . . . . . . 105
6.2 Basic quantities before reconstruction . . . . . . . . . . . . . . . . . 107
6.3 Quality cut distribution . . . . . . . . . . . . . . . . . . . . . . . . . 109
6.4 Angular resolution . . . . . . . . . . . . . . . . . . . . . . . . . . . . 112
6.5 E ective area . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 114
6.6 Point-source sensitivity . . . . . . . . . . . . . . . . . . . . . . . . . . 116
7 Performance of dierent detector designs 119
7.1 Angular resolution . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120
7.2 E ective area . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 122
7.3 Point-source sensitivity . . . . . . . . . . . . . . . . . . . . . . . . . . 124
7.4 E ect of the atmospheric muon background on the multiPMT design 124
8 Scaling of the multiPMT design 129
8.1 Doubling the number of strings . . . . . . . . . . . . . . . . . . . . . 129
8.2 E ects of varying string distances . . . . . . . . . . . . . . . . . . . . 134
8.2.1 Angular resolution . . . . . . . . . . . . . . . . . . . . . . . . 134
8.2.2 E ective area . . . . . . . . . . . . . . . . . . . . . . . . . . . 134
8.2.3 Point-source sensitivity . . . . . . . . . . . . . . . . . . . . . 134
8.2.4 Discovery potential for SNR RX J1713.7{3946 . . . . . . . . 139
Summary and conclusions 141
Zusammenfassung und Ausblick 145
Bibliography 151
7Introduction
It is impressive how extensive our knowledge about the universe and its contents
has become by just looking at the night sky. Astronomy has come a long way
from its beginnings with observations using the naked eye to modern times, where
sophisticated instruments are used to record the information reaching us from the
stars, galaxies and from the host of other amazing things that exist out there. Until
recent times, this information has almost exclusively been measured by detecting
photons, either at optical wavelengths or at other bands including radio, x-rays and
-rays.
There are, however, other particles that reach us, that, until recently, have not
been used to look at the universe. One example is the ux of charged, high-energy
protons and nuclei that are continuously hitting our atmosphere. As it is the case
1so often, the discovery of these particles (being a major part of what has been
called \cosmic rays"), posed more new questions than it answered: Where do these
particles come from? How are they accelerated to the extremely high energies that
we observe?
This thesis was written to be part of a tiny step towards answering these questions.
Even though it is impossible to deduce the origin of most of these charged particles
when they arrive at Earth because their trajectories have been altered by interstellar
magnetic elds, it is nevertheless possible to \see" cosmic ray sources by using two
other types of messengers that are produced in association with them: TeV--rays
and neutrinos. Both of them being uncharged, they can be used to deduce their
source’s origin and, thus, the origin of cosmic rays. TeV--ray astronomy has come
a long way in the recent years, especially thanks to the H.E.S.S. experiment which
was able to produce whole sky maps of sources, some of th