1. Introduction

2. Observations and Data Processing

3. The ICA Technique
3.1. Expected Sources at 3.6 and 4.5 µm and Their Colors
3.2. Independent Component Analysis
3.3. Notation

4. S⁴G Pipeline 5
4.1. Defining the ICA solution area
4.2. Deciding Whether ICA Should be Applied
4.3. Iterative ICA: Reducing the Number of Sources of Emission
4.4. Determining significant secondary emission: thresholding
4.5. Choosing the best solution
4.6. Solution post processing
4.7. Quantifying uncertainties
4.8. Quality flagging

5. Stellar mass maps and products released
5.1. Converting to stellar mass maps
5.2. Public data products

6. Final sample with ICA solutions

7. Results
7.1. Trends with Hubble type
7.2. Trends with SFR
7.3. Global stellar mass estimates at 3.6 µm

8. Summary and Conclusions