FIR fine-structure lines

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Table of contents

1 The Interstellar Medium of Dwarf Galaxies 
1.1 Galaxy
1.2 Phases of the Interstellar Medium
1.2.1 Ionized phase
1.2.2 Neutral atomic phase
1.2.3 Molecular phase
1.2.4 Observational tracers
1.2.5 Dust phase
1.3 Metallicity
1.4 Dwarf galaxies
1.4.1 Stellar population
1.4.2 Star formation
1.4.3 Cloud structure
1.4.4 Dust properties
1.5 Dwarf Galaxy Survey
1.5.1 DGS analysis
1.5.2 Dust properties
1.5.3 Gas properties
1.6 The dwarf irregular galaxy IC10
2 Infrared telescopes: Spitzer, Herschel & SOFIA 
2.1 Infrared observations
2.2 The Spitzer Space Telescope
2.2.1 Spitzer Mission
2.2.2 IRAC
2.2.3 MIPS
2.2.4 IRS
2.2.5 Data reduction – Spitzer/IRS
2.3 The Herschel Space Observatory
2.3.1 Herschel Mission
2.3.2 SPIRE
2.3.3 PACS
2.3.4 Data reduction – Herschel/PACS
2.4 SOFIA Telescope
2.4.1 SOFIA overview
2.4.2 FIFI-LS
2.4.3 SOFIA IC 10 observations
3 Spitzer and Herschel Observations of IC 10 
3.1 Dataset
3.1.1 Spitzer/IRS maps
3.1.2 Herschel maps
3.2 Spatial distribution of ISM tracers
3.2.1 Available tracers
3.2.2 MIR and FIR ratios
3.2.3 Conclusion
4 Modeling the ISM physical properties with Cloudy 
4.1 State-of-the-art modelling
4.1.1 Radiative transfer theory and energy balance
4.1.2 Photoionization models
4.2 Photoionization and photodissociation code: CLOUDY
4.2.1 Overview
4.2.2 Input parameters
4.3 Cloudy models applied to IC10
4.3.1 Setting the input parameters
4.3.2 Stopping criteria
5 Modeling the ionized gas at different spatial scales
5.1 Tracers used
5.2 Spatial decomposition
5.2.1 Description of the spatial scales used
5.2.2 Disentangling the “clumps”
5.3 Building a set of observational constraints for the models
5.3.1 Foreword on the available methods
5.3.2 Line Ratio Method
5.3.3 Absolute Flux Method
5.4 Conclusion