Table 7: Final abundance ratios [X/Fe] of the program stars, compared to those of the metal-poor bulge clusters UKS 1 (Origlia et al. 2005) and Terzan 4 (Origlia et al. 2004). In the 2nd column the solar abundances adopted are reported. No. corresponds to the number of lines used.
Species $\epsilon$(X)$_{\odot}$ No. HP1-2 HP1-3 Mean UKS 1 Terzan 4
$\rm [Fe/H]$ 7.50 50 -1.00 -0.97 -0.99 -0.78 -1.60
$\rm [OI/Fe]$ 8.77 1 +0.40 +0.40 +0.40 +0.27 +0.55
$\rm [NaI/Fe]$ 6.33 2 +0.00 +0.00 +0.00 - -
$\rm [MgI/Fe]$ 7.58 4 +0.00 +0.20 +0.10 +0.32 +0.41
$\rm [SiI/Fe]$ 7.55 8 +0.30 +0.30 +0.30 +0.28 +0.55
$\rm [CaI/Fe]$ 6.36 16 -0.04 +0.10 +0.03 +0.38 +0.53
$\rm [TiI/Fe]$ 5.02 17 +0.04 +0.00 +0.02 +0.32 +0.43
$\rm [TiII/Fe]$   3 +0.10 +0.15 +0.13 -  
$\rm [BaII/Fe]$ 2.13 2 +0.10 +0.20 +0.15 -  
$\rm [LaII/Fe]$ 1.22 1 0.00 0.00 +0.00 -  
$\rm [EuII/Fe]$ 0.51 1 +0.00 +0.30 +0.15 -  


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