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Table of contents
1 Introduction
1.1 The Large Magellanic Cloud in a cosmological context
1.1.1 The Large Magellanic Cloud within the Local Group
1.1.2 LMC-like galaxies in a ΛCDM context
1.2 The Large Magellanic Cloud: morphology, interaction history and chemical evolution
1.2.1 Morphology and kinematics
1.2.2 Stellar populations: observational facts
1.2.2.1 Globular clusters
1.2.2.2 Field stars
1.2.2.3 Detailed chemical abundances
1.2.3 Possible chemical evolution scenarios
1.2.4 Possible dynamical scenarios
1.2.5 Insights on the nature and origin of the LMC bar
1.3 Aims and structure of this thesis work
2 Observations & data processing
2.1 Observations
2.1.1 The FLAMES/GIRAFFE spectrograph
2.1.2 The LMC bar sample
2.1.3 The LMC inner disc sample: re-analysis of Pompeia et al.
2.2 Data processing
2.2.1 Extraction of astronomical spectra
2.2.1.1 Instrumental signatures
2.2.1.2 Spectra extraction
2.2.1.3 Wavelength calibration
2.2.1.4 Putting it all together
2.2.2 Effects of the atmosphere
2.2.2.1 Sky continuum and emission lines
2.2.2.2 Telluric absorption bands
2.2.3 Noise and signal-to-noise ratio measurements
2.2.4 Radial velocities measurements
2.2.4.1 Method to determine the radial velocities
2.2.4.2 Radial velocity measurements for the LMC bar sample
2.2.4.3 Re-determination of the radial velocities for the LMC inner disc sample
2.2.5 Co-addition of spectra and signal-to-noise ratio
2.3 Arcturus as a benchmark star
2.3.1 Principle and aims of differential chemical analysis
2.3.2 Preparation of Arcturus GIRAFFE-like spectra
2.3.3 Discussion on signal-to-noise ratio measurements
2.4 Large tables
3 Stellar parameters determination
3.1 Introduction
3.2 Effective temperature
3.2.1 Definition
3.2.2 How to determine effective temperature?
3.2.3 Photometric temperature of our LMC stars
3.3 Surface gravity
3.3.1 Definition
3.3.2 How to determine surface gravity?
3.3.3 Isochrone gravities of our LMC stars
3.4 Overall metallicity
3.4.1 Definition
3.4.2 Metallicity of our LMC bar stars
3.5 Microturbulence velocity
3.5.1 Definition
3.5.2 How to determine microturbulence velocity?
3.5.3 Microturbulence velocity and metallicity of our LMC stars
3.6 Choice of the reddening
3.7 [Fe/H]CaT vs. [Fe/H]spec
3.8 Large tables
4 Abundance analysis
4.1 From absorption lines to chemical abundances
4.1.1 Concept
4.1.2 Radiative transfer
4.1.3 Line profile
4.1.3.1 Microscopic effects
4.1.3.2 Macroscopic effects
4.1.4 Curve of growth
4.1.5 Notation
4.2 Abundance analysis of our LMC bar and disc stars
4.2.1 Procedures of abundance measurements
4.2.2 Line lists: compilation and calibration
4.2.3 Application to Arcturus
4.2.4 The LMC bar sample
4.2.5 The LMC disc sample
4.2.5.1 Abundances
4.2.5.2 Signal-to-noise ratio for our LMC inner disc stars .
4.3 Error budget
4.3.1 Abundance measurement
4.3.2 Atomic data and line modelling
4.3.3 Stellar parameters
4.4 Correlations between abundance ratios and stellar parameters
5 The chemical history of the Large Magellanic Cloud
5.1 An introduction to galaxy chemical evolution
5.1.1 Stars as chemical element factories
5.1.2 Nucleosynthesis of elements lighter than iron
5.1.2.1 Main sequence evolution
5.1.2.2 Post-main sequence evolution
5.1.3 Iron-peak elements production by type Ia supernova
5.1.4 Nucleosynthesis of elements heavier than the iron-peak
5.1.4.1 AGB nucleosynthesis: s-process
5.1.4.2 Explosive nucleosynthesis: r-process
5.1.5 From stellar nucleosynthesis to galactic chemical evolution .
5.2 The chemical evolution of the LMC
5.2.1 A slow chemical evolution
5.2.2 Is the LMC IMF different?
5.2.3 Do we need prompt type Ia supernovae?
5.3 Chemical anomalies: new lights on nucleosynthesis models
5.4 A new picture for the formation of the LMC bar
6 Conclusion & future works
6.1 Main developments for this thesis work
6.2 Main results of this thesis work
6.3 Future works
A Final line lists
B Final abundances for LMC bar stars
C Final abundances for LMC bar stars
D Publications
Bibliographies
