(Downloads - 0)
For more info about our services contact : help@bestpfe.com
Table of contents
Introduction
I Scientific Framework
1 Quantum gravity and departures from Lorentz invariance tested with photons from astrophysical sources
1.1 Quantum gravity built on effective field theories
1.1.1 String theories
1.1.2 Loop quantum gravity
1.2 Departures from Lorentz invariance
1.2.1 Breaking Lorentz symmetry
1.2.2 Deforming Lorentz symmetry
1.3 Phenomenology
1.3.1 Time delays
1.3.2 Kinematic interactions and threshold effects
1.4 Astrophysical probes
1.4.1 Gamma-ray bursts
1.4.2 Pulsars
1.4.3 Flaring active galactic nuclei
1.5 LIV vs source intrinsic effects
2 Blazars
2.1 Characteristics
2.1.1 Superluminal motion and relativistic beaming
2.1.2 Blazar emission
2.1.3 Blazar sequence: BL Lac vs. FSRQ
2.2 Physical processes in relativistic jets
2.2.1 Acceleration
2.2.2 Leptonic radiation processes
2.2.2.1 Synchrotron
2.2.2.2 Inverse Compton
2.2.2.3 External inverse Compton
3 Gamma-ray astronomy with imaging atmospheric Cherenkov telescopes
3.1 VHE gamma-ray astronomy
3.1.1 Direct detection: satellite-embarked instruments
3.1.2 Indirect detection: ground-based imaging atmospheric Cherenkov telescopes
3.1.2.1 Extensive air showers
3.1.2.2 Cherenkov radiation
3.1.2.3 Imaging atmospheric Cherenkov telescopes
3.2 H.E.S.S.: the high energy stereoscopic system
3.2.1 Overview of the H.E.S.S. array
3.2.2 Structure and optical system
3.2.3 Data acquisition
3.2.3.1 Trigger system
3.2.3.2 Calibration
3.2.4 Analysis
3.2.4.1 Event reconstruction
3.2.4.2 Signal extraction
3.2.4.3 Spectral and temporal analysis
3.3 CTA: the Cherenkov telescope array
II Modelisation of blazar emission and interpretation of intrinsic delays
4 Intrinsic time delays in blazars
4.1 Time-dependent modeling of blazar
4.1.1 Generating a flare
4.1.1.1 Homogeneous one-zone SSC model
4.1.1.2 Extended scenario
4.1.1.3 Domains of parameters
4.1.2 Generating astrophysical observables: the AGNES simulator
4.1.2.1 Lepton spectrum
4.1.2.2 Energy spectrum
4.1.2.3 Light curves and intrinsic time delays
4.2 Properties of intrinsic time delays
4.2.1 Regimes in the SSC scenario
4.2.2 Impact of model parameters on intrinsic delays
4.2.2.1 SSC scenario
4.2.2.2 Extended scenario
4.2.3 Observability of non-zero intrinsic delays
5 Discrimination between intrinsic and LIV-induced time delays
5.1 Multi-frequency study: gamma-rays vs. X-rays
5.1.1 Euclidian distance study
5.1.1.1 Building a powerful tool
5.1.1.2 Dependency on model parameters
5.1.2 Hysteresis study: a sensitive tool
5.2 LIV injection
5.2.1 Impact on delays and euclidian distances
5.2.2 Impact on hysteresis
5.3 LIV-modified EBL absorption: extreme scenarii
5.4 Observational perspectives
III Preparation for population studies with VHE data
6 Searches for Lorentz invariance violation signatures with time of flight studies
6.1 Analysis methods
6.1.1 Single data set transformation
6.1.2 Comparison between data subsets
6.1.3 Strengths and limitations
6.2 State of the art
6.2.1 Up-to-date limits
6.2.2 Future prospects
7 Method development and validation for future population studies
7.1 The maximum likelihood method
7.1.1 Building a probability density function
7.1.2 The special case of pulsars
7.1.3 Background treatment
7.1.4 IRF treatment
7.1.4.1 Acceptance
7.1.4.2 Energy resolution
7.1.4.3 Multi-era treatment
7.1.4.4 Optimising the computational time
7.1.5 Combination
7.1.6 Confidence intervals
7.2 Lag distance models
7.3 Selected sources and simulation parameters
7.4 Tests and calibration
7.4.1 At n = 0: tabulation settings
7.4.2 For n 6= 0: calibration
7.5 Statistical and systematic uncertainties
7.6 Results and discussion on the QG energy scale
7.6.1 Individual sources and combinations
7.6.2 Subluminal vs. superluminal
7.6.3 Systematic uncertainties
7.6.4 Lag-distance models
7.6.5 Comparison with older published limits (subluminal)
7.7 Summary and perspective
Conclusion
A Solution of the time dependent SSC differential equation
B Convergence and calibration plots produced with the LIVelihood software
Bibliography
