Gas velocity dispersion and the energy sources

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Table of contents

1 Introduction 
1.1 Star formation: the driver of galaxy evolution
1.2 Star formation obscured by interstellar dust
1.2.1 Multi-wavelength study of galaxies
1.2.2 The main sequence of star-forming galaxies
1.2.3 Cosmic star formation history
1.2.4 Observing star-forming galaxies in the (sub)millimeter
1.2.5 Optically-dark galaxies
1.3 Star formation fueled by gas
1.3.1 Gas tracers
1.3.2 Star formation law
1.3.3 Gas content
1.4 Star formation as one of the energy sources of gas
1.4.1 Gas velocity dispersion and the energy sources
1.4.2 Integral field unit (IFU), datacube and beam smearing effect
2 Summary of the work done in this thesis 
2.1 GOODS-ALMA
2.1.1 Optically dark galaxies and their association with a proto-cluster in formation at z ≥3.5
2.1.2 Data compilation
2.1.3 Nascent AGNs in GOODS-ALMA
2.1.4 Contribution as third author
2.2 Extremely metal-poor galaxies
2.2.1 Spatially resolved dust emission
2.2.2 Gas content in IZw18
2.3 The SAMI Integral field Units (IFU) Survey
2.3.1 Energy source of turbulence in star-forming galaxies
2.4 Observations
3 GOODS-ALMA: optically-dark ALMA galaxies shed light on a cluster in formation at z = 3.5 
3.1 Introduction
3.2 Data and observations
3.2.1 ALMA data and observations
3.2.2 Ancillary data
3.2.3 Origin of the redshifts and stellar masses
3.2.4 Derived parameters of the optically dark galaxies
3.3 Results of the ALMA spectroscopic follow-up
3.3.1 AGS4
3.3.2 AGS17
3.3.3 Upper limits of AGS11, AGS15 and AGS24
3.4 GOODS-ALMA optically-dark galaxies
3.4.1 AGS4, an extremely massive galaxy at z=3.556 and a case of blending in the Hubble H-band image
3.4.2 AGS25, the most distant optically-dark galaxy in GOODS-ALMA
3.5 An over-density at z ≥3.5 in GOODS-ALMA
3.5.1 Clustering properties of optically dark galaxies
3.5.2 A clear peak at z ≥3.5 in the redshift distribution
3.5.3 Optically-dark galaxies at z ≥3.5
3.5.4 Spatial distribution of galaxies at z ≥3.5 in the GOODS-ALMA field
3.5.5 Dynamical state of the proto-cluster at z ≥3.5
3.6 Conclusions
4 Extremely weak CO emission in IZw 18 
4.1 Introduction
4.2 Observations
4.3 Results
4.3.1 CO J=2-1
4.3.2 1.3mm continuum
4.4 Discussion
4.4.1 SED and Submilimetre excess
4.4.2 Infrared luminosity and SFR versus LÕCO
4.4.3 The structure of the interstellar medium
4.5 Conclusion
5 The SAMI Galaxy Survey: energy sources of the turbulent velocity dispersion in spatiallyresolved local star-forming galaxies 
5.1 Introduction
5.2 Sample and data analysis
5.2.1 Sample selection
5.2.2 Gas kinematic information
5.2.3 Spatial resolution
5.3 Results
5.3.1 The spatial distribution of !SFR, vgas, and ‡gas
5.3.2 The ‡gas – !SFR relation in local and high redshift star-forming galaxies
5.4 Discussion
5.4.1 Main driver(s) of velocity dispersion
5.4.2 Caveats
5.5 conclusion
6 Spatially resolved dust emission of extremely metal poor galaxies1 
6.1 Introduction
6.2 Sample, observations and data analysis
6.2.1 The sample
6.2.2 Observations
6.2.3 Photometric measurements
6.3 The far-IR SEDs
6.3.1 The color-color diagrams
6.3.2 Modified black-body fitting
6.3.3 Spatial variations of SEDs and dust heating Mechanism
6.4 Dust-to-stellar mass ratio
6.5 Conclusions
7 Conclusion and perspectives 
7.1 Conclusion
7.2 Perspective
7.2.1 More on the optically dark galaxies
7.2.2 AGN feedback on high-z star-forming galaxies
Bibliography