High-energy emission from bright gamma-ray bursts using fermi [Elektronische Ressource] / Elisabetta Bissaldi

Pgoehringer

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• Physik

Informations

• Publié par: technische_universitat_munchen
• Publié le: 01 janvier 2010
• Nombre de lectures: 18
• Poids de l'ouvrage: 9 Mo

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PHYSIK-DEPARTMENT




High-Energy Emission from Bright
Gamma-Ray Bursts using Fermi


Dissertation
von

Elisabetta Bissaldi








TECHNISCHE UNIVERSITÄT MAX-PLANCK-INSTITUT
MÜNCHEN FÜR EXTRATERRESTRISCHE PHYSIK TECHNISCHE UNIVERSITÄT
MÜNCHEN
Max–Planck–Institut für extraterrestrische Physik
High−Energy Emission from Bright
Gamma–Ray Bursts using Fermi
Elisabetta Bissaldi
Vollständiger Abdruck der von der Fakultät für Physik der Technischen Universität
München zur Erlangung des akademischen Grades eines
Doktors der Naturwissenschaften
genehmigten Dissertation.
Vorsitzender: Univ.–Prof. Dr. A. Ibarra
Prüfer der Dissertation: 1. Hon.–Prof. Dr. G. Hasinger
2. Univ.–Prof. Dr. L. Oberauer
Die Dissertation wurde am 08.04.2010 bei der Technischen Universität München
eingereicht und durch die Fakultät für Physik am 25.05.2010 angenommen.To my dadContents
List of Figures IV
List of Tables VIII
Summary and Dissertation Outline 1
Zusammenfassung 3
1 Gamma–Ray Bursts: An Overview 7
1.1 The “Dark” Era . .......................... 8
1.2 TheBATSEEra ........................... 11
1.2.1 GRB Global Properties ................... 12
1.2.2 EGRET and the High–Energy GRB Emission ....... 19
1.3 The Afterglow Era 22
1.3.1 Important Observational Progress . . ........... 23
1.3.2 Theoretical GRB Models . . . ............... 25
1.3.3 GRB Relationships . . 30
1.4 The Pre–FermiEra ......................... 33
1.4.1 The Swift Mission . . . ................... 34
2 The Fermi Observatory 37
2.1 The Large Area Telescope . . 38
2.1.1 Precision Converter–Tracker . ............... 41
2.1.2 Calorimeter . . . . . . 42
2.1.3 Anticoincidence Detector . . . 43
2.1.4 LAT and GRBs . . . . ................... 45
2.2 The Gamma–Ray Burst Monitor . . . 48
2.2.1 NaI(Tl) Detectors . . . 48
2.2.2 BGO . . . . 50
2.2.3 PMTs and FEE . . . . 52
ICONTENTS
2.2.4 Data System . ........................ 54
2.3 GBM Triggers ............................ 56
2.3.1 Trigger localization . .................... 56
2.3.2 Spacecraft Reorientations . . ................ 58
2.3.3 TRIGDAT . . 61
2.3.4 The RMFIT Analysis Software . . . ............ 62
3 GBM Performance 63
3.1 Calibration Campaigns . . . .................... 64
3.1.1 MPE Laboratory Setup and Instrumentation ........ 66
3.1.2 NaI Low–Energy Calibration at PTB/BESSY . . . .... 68
3.1.3 BGO High–Energy at SLAC . . 69
3.1.4 Simulation of the Laboratory and the Calibration Setup . . 71
3.2 Calibration Data Analysis . . 73
3.2.1 Database and software . . . ................ 73
3.2.2 Processing of Calibration Runs . . . ............ 73
3.3 Calibration Results . ........................ 87
3.3.1 Channel–to–Energy (CE) Relation . 87
3.3.2 Energy Resolution . ....................109
3.3.3 Full–Energy Peak Effective Area and Angular Response . 116
3.3.4 QDE and Spatial Uniformity of NaI Detectors . . . ....121
3.3.5 NaI Detectors High–Voltage dependence . . ........125
3.3.6 NaI EQM Thermal Test . . . ................127
3.4 Detector Calibration at System Level28
3.4.1 Channel–to–Energy Conversion . . ............130
3.5 On–Orbit Performance and Operations . . .31
4 First Year of GBM Scientific Results 135
4.1 GRB 090323 and GRB 090328 . . . ................136
4.1.1 Observations of GRB 09032337
4.1.2ations of GRB 09032839
4.1.3 Time–Resolved Spectral Analysis . ............141
4.2 Joint GBM–LAT Observations . . .44
4.3 GRB 090902B............................157
4.3.1 Observations and Light Curves . . .57
4.3.2 Time–resolved Spectral Analysis . . ............159
4.3.3 Discussion and Interpretation................162
IICONTENTS
4.4 GBM and BAT Observations of GRB 080810 ...........165
4.4.1 Observations and Analyses . . ...............166
5 BGO–Bright GRBs 173
5.1 Selection Methodology . . . . ...................174
5.1.1 Event Selection . . . .74
5.1.2 Detector . .76
5.1.3 Data Type Selection . .76
5.1.4 Time and Energy Interval Selections . ...........177
5.2 Analysis of the BGO Peak Count Rate ...............180
5.2.1 LAT Detections . . . . ...................187
5.2.2 BGO Effective–Area Correction . . .89
5.3 Spectral Analysis ..........................190
5.3.1 Photon Models . . . .90
5.4 Spectral Analysis Results . . .93
5.4.1 Spectral Parameter Distribution...............198
5.4.2 Correlation Among Spectral Parameters . . . .......207
Conclusions 215
Bibliography 217
IIIList of Figures
1.1 Light curve of the first Gamma–Ray Burst . . . ........ 9
1.2 Temporal variations in GRB 821104 . . ............ 10
1.3 Isotropic distribution of 2704 BATSE GRBs . . ........ 13
1.4 Bimodal distribution of BATSE GRBs . 14
1.5 Distribution of hardness ratio versus T 1590
1.6 GRB light curves from the first BATSE Catalog ........ 15
1.7 Deconvolved spectra of GRB 990123 . ............ 16
1.8 Spectral parameter distributions from BATSE GRBs . .... 18
1.9 High–energy emission from GRB 940217 . . . ........ 19
1.10 Energy fluxes for GRB 941017 . ................ 21
1.11 Beppo-SAX observation of GRB 970228 . . . ........ 24
1.12 V–band images of the GRB 970228 optical afterglow . .... 24
1.13 Schematic diagram of the fireball shock model ........ 29
1.14 E –E distribution . . . .................... 31p iso
1.15 Energy fluence–E distribution................ 32peak
1.16 Effective areas for Swift and Fermi detectors . . ........ 35
2.1 The launch of the Fermi Observatory . . ............ 38
2.2 Schematic diagram of the Large Area Telescope ........ 39
2.3 The LAT tracker ........................ 41
2.4 LAT calorimeter module .................... 43
2.5 LATACD ............................ 44
2.6 GRB localization with the LAT . ................ 46
2.7 Model–dependent LAT GRB sensitivity ............ 47
2.8 GBM NaI detector . . . 49
2.9 X–ray transmission of the NaI detector entrance window . . . 51
2.10 The Fermi spacecraft . . .................... 51
2.11 GBM BGO detector . . . 53
2.12 Functional block diagram of GBM . . . ............ 55
IV