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Table 6:

Comparison of our results for star 141 in M 67 with the analysis of Tautvaisiene (2000) and Yong et al. (2005).

Parameter
Here T00 Y05
Resolution 30 000 30-60 000 28 000
S/N 70-100 $\geq$100 30-100
$T_{\rm {eff}}$ (K) 4650 4730 4700
log g (dex) 2.8 2.4 2.3
vt (km s-1) 1.3 1.8 1.3
[FeI/H] 0.06 $\pm$ 0.01($\pm$0.10) -0.01 $\pm$ 0.02 -0.01 $\pm$ 0.02
[FeII/H] 0.01 $\pm$ 0.03($\pm$0.10) -0.01 $\pm$ 0.05 0.01 $\pm$ 0.03
[$\alpha $/Fe] 0.01 $\pm$ 0.01($\pm$0.07) 0.01 $\pm$ 0.03 0.12 $\pm$ 0.06
[Al/Fe] 0.06 $\pm$ 0.06($\pm$0.05) 0.08 $\pm$ 0.01 0.16 $\pm$ 0.03
[Ba/Fe] 0.26 $\pm$ 0.05($\pm$0.06) 0.07 $\pm$ 0.00 0.02 $\pm$ 0.00
[Ca/Fe] -0.13 $\pm$ 0.02($\pm$0.03) 0.09 $\pm$ 0.05 0.09 $\pm$ 0.02
[Co/Fe] 0.11 $\pm$ 0.02($\pm$0.06) 0.05 $\pm$ 0.07 0.01 $\pm$ 0.05
[Cr/Fe] 0.01 $\pm$ 0.03($\pm$0.06) 0.12 $\pm$ 0.05 -
[La/Fe] 0.06 $\pm$ 0.05($\pm$0.09) -0.06 $\pm$ 0.00 0.13 $\pm$ 0.03
[Mg/Fe] 0.29 $\pm$ 0.03($\pm$0.10) 0.11 $\pm$ 0.00 0.18 $\pm$ 0.02
[Na/Fe] 0.10 $\pm$ 0.02($\pm$0.04) 0.25 $\pm$ 0.00 0.24 $\pm$ 0.06
[Nd/Fe] 0.01 $\pm$ 0.29($\pm$0.10) - -
[Ni/Fe] 0.06 $\pm$ 0.02($\pm$0.03) 0.05 $\pm$ 0.04 0.06 $\pm$ 0.03
[O/Fe] -0.05 $\pm$ 0.09($\pm$0.08) 0.04 $\pm$ 0.00 0.10 $\pm$ 0.04
[Sc/Fe] -0.02 $\pm$ 0.08($\pm$0.08) 0.09 $\pm$ 0.05 -
[Si/Fe] 0.09 $\pm$ 0.02($\pm$0.08) 0.11 $\pm$ 0.04 0.11 $\pm$ 0.04
[TiI/Fe] -0.07 $\pm$ 0.02($\pm$0.07) 0.04 $\pm$ 0.05 0.05 $\pm$ 0.03
[TiII/Fe] -0.07 $\pm$ 0.08($\pm$0.06) 0.11 $\pm$ 0.07 -
[V/Fe] 0.13 $\pm$ 0.04($\pm$0.14) 0.09 $\pm$ 0.03 -
[Y/Fe] -0.04 $\pm$ 0.02($\pm$0.12) -0.12 $\pm$ 0.08 -

Notes. The internal uncertainties are those reported by the authors, where a value of 0.00 means that the abundance calculation was based on one line only.


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