1. INTRODUCTION

2. OBSERVATIONS AND DATA  
2.1. Data Reduction and Control Fields  
2.2. WFPC2 Parallel Fields  

3. CALCULATING SPECIFIC FREQUENCIES, LUMINOSITIES, AND MASSES  
3.1. Total Numbers of GCs  
3.2. Total Luminosities and Masses of GCs  
3.4. Stellar Mass  

4. RESULTS  
4.1. \(S_{N}\) versus Galaxy Magnitude  
4.2. \(S_{N,z}\) and Bulge Luminosity  
4.3. Normalizing to Stellar Mass  
4.4. Specific Luminosity and Mass  
4.5. Specific Frequencies of Red and Blue GCs  
4.6. \(S_{N,z}\) and Nucleation  
4.7. \(S_{N,z}\) and Environment  

5. DISCUSSION  
5.1. Mass Dependence of the GC Mass Fraction  
5.2. Environment and Biased GC Formation  
5.3. Possible Mechanisms for Quenching Star Formation  
5.4. Globular Cluster Destruction  
5.5. \(S_{N}\) Variation in Metal-poor and Metal-rich GCs  

6. CONCLUSIONS