1 INTRODUCTION  
2 METHODS AND DATA  
2.1 Calculating better distances to open clusters  
2.2 Calculating photometric stellar parameters  
2.3 Spectroscopic fitting  
3 RESULTS  
3.1 Distance improvements  
3.2 Isochrone fitting and photometric stellar parameters  
3.3 Abundances  
4 SPECTROSCOPIC PRECISION  
5 DISCUSSION  
6 CONCLUSIONS