1. INTRODUCTION  
2. DATA  
3.1. SFHs and stellar population properties  
3.2. $D_{n}$ 4000-H δ $A$ comparison of training library to MaNGA spaxels  
3.3. Why not use CMLRs?  
4. PARAMETER ESTIMATION IN THE PCA FRAMEWORK  
5. RESOLVED STELLAR MASS-TO-LIGHT RATIOS: DISCUSSION AND CONCLUSION