1. Introduction

2. Scientific Motivation
2.1. The Importance of MIR Spectroscopy
2.2. MIR Spectral Diagnostics

3. Sample Definition and Properties
3.1. The Lockman Hole
3.2. Selection Criteria
3.3. Sample Properties

4. Instrument, Observing Mode, and AORs
4.1. Low-Resolution IRS Spectroscopy
4.2. High-Resolution IRS Spectroscopy
4.3. Slit Positions
4.4. Peak-up Imaging
4.5. Solar Flare

5. Data Reduction
5.1. Low-Resolution Spectroscopy
5.2. High-Resolution Spectroscopy
5.3. Achieved Sensitivity

6. SSGSS Data
6.1. Low-Resolution Spectra
6.2. High-Resolution Spectra
6.3. Emission Line Strengths
6.4. Composite Spectra

7. Results and Discussion
7.1. Comparison to Starburst Spectra
7.2. Comparison of Absorption and Continuum Properties
7.3. PAH Contribution to the IR Luminosity
7.4. Dust Mass

8. Data Products and Value-Added Catalogs
8.1. Spitzer Data Archive
8.2. Complementary Data Products

9. Summary