1. INTRODUCTION

2. PLANET FORMATION AND ACCRETION  
2.1. Observational Evidence for the Relation Between M and M  
2.2. M as a Probe of Formation Pathways  
2.3. Total Accretion Luminosity  
2.4. Accretion Mechanisms and H α Emission  
2.5. Modeling Planetary Orbits  

3. DATA

4. METHOD TO COMPUTE COMPLETENESS  
4.1. Simulating Accretion Rates  
4.2. Computing H α Luminosity  
4.3. Orbital Distributions  
4.4. Detectability  

5. RESULTS AND DISCUSSION  
5.1. GAPlanetS Completeness to Accreting Objects  
5.2. Constraints on Protoplanet Occurrence Rate  

6. CONCLUSION