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Table 3.

Abundances of the observed stars.

Elements 1 2 3 4 5 6 7 Cluster Sun
[O/Fe] 0.07 0.00 0.31 0.15 0.11 −0.09 −0.09 +0.07 ± 0.05 8.83
±0.03 ±0.04 ±0.04 ±0.06 ±0.05 ±0.03 ±0.05
[Na/Fe]NLTE 0.10 −0.02 0.31 0.75 0.82 0.60 0.19 +0.39 ± 0.13 6.32
±0.08 ±0.07 ±0.06 ±0.07 ±0.06 ±0.04 ±0.07
[Mg/Fe] 0.34 0.37 0.24 0.20 0.29 0.28 0.11 +0.26 ± 0.03 7.56
±0.03 ±0.05 ±0.05 ±0.06 ±0.07 ±0.04 ±0.06
[Al/Fe] 0.44 0.32 0.54 0.56 0.49 0.40 0.33 +0.44 ± 0.04 6.43
± 0.04 ±0.04 ±0.04 ±0.05 ±0.07 ±0.04 ±0.05
[Si/Fe] 0.16 −0.17 −0.06 0.20 −0.10 −0.07 −0.12 −0.02 ± 0.05 7.61
±0.08 ±0.06 ±0.06 ±0.07 ±0.06 ±0.04 ±0.08
[Ca/Fe] 0.01 −0.10 0.02 0.02 0.10 0.21 −0.05 +0.03 ± 0.04 6.39
±0.07 ±0.06 ±0.04 ±0.06 ±0.05 ±0.05 ±0.06
[Sc/Fe] 0.32 0.22 0.38 0.41 −0.12 0.04 0.11 +0.19 ± 0.07 3.12
±0.07 ±0.06 ±0.06 ±0.07 ±0.07 ±0.04 ±0.07
[Ti/Fe] 0.44 0.24 0.47 0.52 0.60 0.73 0.45 +0.49 ± 0.06 4.94
±0.03 ±0.04 ±0.04 ±0.06 ±0.05 ±0.06 ±0.06
[V/Fe] 0.13 0.17 0.22 0.19 0.33 0.25 0.23 +0.22 ± 0.02 4.00
±0.06 ±0.06 ±0.06 ±0.06 ±0.05 ±0.04 ±0.06
[Cr/Fe] 0.07 -0.07 0.31 0.10 0.18 0.26 −0.03 +0.12 ± 0.05 5.63
±0.10 ±0.10 ±0.10 ±0.11 ±0.06 ±0.06 ±0.08
[Mn/Fe] 0.40 0.04 0.27 0.04 0.45 0.17 0.08 +0.21 ± 0.06 5.37
±0.09 ±0.07 ±0.09 ±0.09 ±0.07 ±0.08 ±0.09
[Fe/H] −0.16 −0.12 −0.24 −0.11 −0.55 −0.20 −0.03 −0.20 ± 0.06 7.50
±0.03 ±0.02 ±0.02 ±0.03 ±0.04 ±0.03 ±0.03
[Co/Fe] 0.74 0.52 0.64 0.61 0.54 0.83 0.53 +0.63 ± 0.04 4.93
±0.08 ±0.08 ±0.09 ±0.10 ±0.09 ±0.08 ±0.10
[Ni/Fe] 0.25 0.15 0.22 0.16 0.13 0.41 0.22 +0.22 ± 0.04 6.26
±0.05 ±0.06 ±0.08 ±0.06 ±0.06 ±0.08 ±0.08
[Cu/Fe] 0.15 0.01 0.49 0.31 0.44 0.47 0.52 +0.34 ± 0.07 4.19
±0.09 ±0.11 ±0.12 ±0.13 ±0.10 ±0.10 ±0.12
[Zr/Fe] −0.19 −0.22 −0.14 −0.17 −0.05 −0.19 −0.15 −0.16 ± 0.02 2.25
±0.05 ±0.04 ±0.06 ±0.06 ±0.04 ±0.04 ±0.06
[Ba/Fe] 0.04 0.07 0.08 0.06 0.00 0.08 0.10 +0.06 ± 0.01 2.34
±0.06 ±0.05 ±0.06 ±0.07 ±0.04 ±0.04 ±0.06
[Eu/Fe] 0.30 0.25 0.37 0.31 0.13 0.16 0.26 +0.25 ± 0.03 0.52
±0.04 ±0.05 ±0.05 ±0.05 ±0.04 ±0.04 ±0.06

Notes. Columns 2–8: abundances of the observed stars in NGC 6528. Column 9: mean abundance for the cluster; we include the statistical errors obtained from the mean. Column 10: abundances adopted for the Sun in this paper, indicated as logϵ(El.). The errors presented for each abundance, in Cols. 2–8, were calculated by dividing the rms scatter by the square root of the number of the lines used for a given element and a given star. For elements whose abundance was obtained by spectrum synthesis, the error is the output of the fitting procedure.

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