Thermal radio continuum emission

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Table of contents

1 The Interstellar Medium 
1.1 Components of the Interstellar Medium
1.2 Observation of different emissions in the ISM
1.2.1 X-ray and Extreme UV emissions
1.2.2 UV emission
1.2.3 Optical line emission
1.2.4 Infrared emission: radiation by dust
1.2.5 Radio line emission
1.3 Other emissions
1.3.1 γ-ray emission
1.3.2 Thermal radio continuum emission
1.3.3 Non-Thermal synchrotron emission
2 Molecular gas in galaxies 
2.1 Molecular Clouds
2.2 Cloud structure
2.2.1 The Virial Theorem for molecular clouds
2.2.2 Structure analysis techniques
2.2.3 Clumps
2.3 Star formation in molecular clouds
2.4 Molecular gas content
2.4.1 CO-H2 conversion factor
2.4.2 Intensity line ratios
2.5 Distribution and dynamics of the CO
2.5.1 Radial and vertical distribution
2.5.2 Dynamics: bars, shells and tidal dwarfs
2.6 CO as a function of type and environment
2.7 CO at high redshift
3 Relations between ISM tracers 
3.1 Emissions and star formation
3.2 The sample
3.3 Results
3.3.1 Cold gas and warm dust
3.3.2 X-ray component
3.4 Discussion
3.4.1 Late-type galaxies
3.4.2 Early-type galaxies
3.5 Modelling early-type galaxies
3.5.1 The galactic radius and mass of stars and gas
3.5.2 The scale radii
3.5.3 The star formation history
3.6 Conclusions
4 Messier 81 
4.1 The idea
4.2 Observations
4.3 Molecular gas emission
4.3.1 A and B receivers
4.3.2 HERA receiver
4.3.3 Line ratio
4.4 Clumping properties of the gas
4.4.1 Molecular Associations
4.4.2 GMAs masses
4.4.3 Virial equilibrium
4.4.4 The X factor for M 81
4.5 Comparison with previous works
4.6 Discussion
4.6.1 The X problem
4.6.2 Heating of the gas
4.7 Conclusions
4.8 Future perspectives
5 NUGA survey: NGC 3147 
5.1 NUGA project
5.1.1 Aims and results already obtained
5.2 NGC 3147 galaxy
5.3 Observations
5.3.1 IRAM single dish CO and HCN observations
5.3.2 IRAM interferometer CO observations
5.3.3 Near-infrared observations
5.3.4 Archival observations with Spitzer and GALEX
5.4 Single dish results
5.5 Interferometric results: Molecular gas properties
5.5.1 Morphology and mass of the CO rings
5.5.2 Kinematics of the CO rings
5.6 Comparison with Spitzer and GALEX
5.7 Computation of the torques
5.7.1 Near infrared images
5.7.2 Evaluation of the gravitational potential
5.7.3 Evaluation of gravity torques
5.8 Discussion
5.9 Conclusions
6 Conclusions and Future Applications 
6.1 Conclusions and obtained results
6.2 The future: ALMA
6.2.1 Synergy between ALMA and Herschel
7 Candidate’s list of papers 
Bibliography