1. INTRODUCTION

2. OBSERVATIONS
2.1. Sample Selection
2.3. FTS Spectral Line Fitting
2.4. Photometry

3. ANALYSIS
3.1. Dust Modeling Likelihood with Multinest
3.2. CO Modeling Likelihood with Multinest
3.4. LTE Analysis of H₂
3.5. [C II] and [N II] Line Ratios

4. DISCUSSION
4.1. Distinct Components vs. a Continuous Distribution
4.2. Luminosity to Mass Conversion Factors
4.3. Gas-to-Dust Mass Ratios
4.4. Molecular Gas Properties in Context: Comparisons Among Galaxies
4.5. Carbon in Various Forms: C, C⁺, CO

5. CONCLUSIONS