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Table of contents
1 Introduction
1.1 Asteroids History
1.1.1 How have they been observed?
1.1.2 Observation Methods and Missions
1.2 Stellar Occultations
1.2.1 General properties
1.2.2 Why are they important?
1.3 The Gaia Mission
1.4 Goals and Structure of this Thesis
2 Extending the occultations sample with Gaia
2.1 Context
2.2 UniversCity Telescope
2.3 Limitations to account for in DR2
2.4 Set-up
2.5 Star and Asteroid Uncertainties
2.6 Orbit improvements with Gaia
2.7 Statistics on events per size
3 Simulations
3.1 Context
3.2 Least Squares and Bayes’ Theorem
3.2.1 Least Squares Fit Method
3.2.2 Bayes’ Theorem and Bayesian Analysis
3.3 Setup
3.4 Results
3.4.1 Gaussian and Uniform priors
3.4.2 False positives
3.4.3 Comparison of BIM to LSF
3.4.4 DIAMONDS vs PyOTE
3.4.5 BIM vs Real Cases
4 Observations
4.1 Context
4.2 Positives
4.2.1 Triton
4.2.2 Aemilia
4.2.3 Phaethon
4.2.4 Millman
4.3 Negatives
4.3.1 2000 HD22
4.3.2 Gezelle
4.3.3 Sveta
4.3.4 Paijanne
4.3.5 Nolde
4.3.6 Modestia
4.3.7 1993 FE48
4.3.8 Deikoon
4.3.9 Elektra
4.3.10 Phaethon
4.3.11 Europa
4.3.12 Alfaterna
4.3.13 2002 MS4
4.4 Analysis to other observations
4.4.1 Europa event – RIO team
4.4.2 Galatea
4.4.3 Euphrosyne
5 Exploiting Occultation Astrometry
5.1 Context
5.1.1 Debiasing
5.1.2 Error Models
5.2 Setup
5.3 Testing error models with occultations
5.3.1 Best occultations
5.3.2 Full Scale Runs on Occultations
5.4 Orbital Elements with Gaia
5.4.1 Full Scale Run on DR2 Asteroids
6 Conclusions and Future Work
6.1 UniversCity and Robotic Telescopes
6.2 Simulation of events
6.3 Comparing astrometry: occultations and other sources
6.4 Future Work
6.4.1 Gaia DR3 and beyond
6.4.2 Exploiting Single Chord Occultations
6.4.3 NEA Events
Bibliography
