| The self-enrichment of galactic halo 
         globular cluster:
         a clue to their formation ? Figure 1. | 

 /Fe] with the 
     data from Jehin et al. (1999) (full squares), the data of Nissen and 
     Schuster (1997) (full triangles), the data of Zhao and Magain (1991) 
     (full pentagon), the data of Edvardsson et al.~(1993) for 
     [Fe/H] < -0.6 
     (full circles) and for [Fe/H] >- 0.6 (open circles).
     The zero points have been fixed by comparing the results obtained for
     the stars in common with Jehin et al. (1999)
/Fe] with the 
     data from Jehin et al. (1999) (full squares), the data of Nissen and 
     Schuster (1997) (full triangles), the data of Zhao and Magain (1991) 
     (full pentagon), the data of Edvardsson et al.~(1993) for 
     [Fe/H] < -0.6 
     (full circles) and for [Fe/H] >- 0.6 (open circles).
     The zero points have been fixed by comparing the results obtained for
     the stars in common with Jehin et al. (1999)