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Table 5

Uncertainties on derived [Mn/Fe] for the metal-poor star B3-b1 and the red clump star BWc-6.

Star T eff log g [Fe/H] v t Ref. [Mn1/Fe] [Mn2/Fe] [Mn3/Fe] [Mn4/Fe] [Mn/Fe]

B3-b1 4300 1.7 –0.78 1.5 1 –0.3 –0.3 (–0.9) –0.3 –0.35
B3-b1 4400 1.7 –0.60 1.3 2 –0.3 –0.3 (–1.0) –0.40 –0.38
B3-b1 4365 2.0 –0.73 1.5 3 –0.3 –0.3 (–0.9) –0.35 –0.37
B3-b1 4150 1.7 –0.78 1.5 –0.4 –0.45 (–1.0) –0.5 –0.50
B3-b1 4300 2.2 –0.78 1.5 –0.3 –0.3 (–0.8) –0.3 –0.35
B3-b1 4300 1.7 –0.78 1.6 –0.3 –0.3 (–0.9) –0.6 –0.35
B3-b1 4300 1.7 –0.88 1.5 –0.15 –0.15 (–0.7) –0.15 –0.20

BWc-6 4787 2.2 –0.35 1.5 1 0.0 +0.1 0.0 0.0 0.03
BWc-6 4769 2.2 –0.17 1.2 4 –0.05 –0.05 –0.1 –0.1 –0.08
BWc-6 4769 2.2 –0.25 1.3 5 –0.1 0.0 –0.05 –0.02 –0.04
BWc-6 4620 2.2 –0.25 1.3 0.0 –0.3 –0.2 –0.25 –0.19
BWc-6 4769 2.7 –0.25 1.3 0.0 0.0 0.0 0.0 0.00
BWc-6 4769 2.2 –0.25 1.4 0.0 0.0 0.0 0.0 0.00
BWc-6 4769 2.2 –0.35 1.3 0.0 0.0 0.0 0.0 0.00

Reference. (1) Lecureur et al. (2007) (present results); (2) Zoccali et al. (2008); (3) Ryde et al. (2010); (4) Hill et al. (2011) GIRAFFE data; (5) Hill et al. (2011) UVES data (present results). [Mn/Fe] is also derived with changes in model parameters of ΔTeff = −150 K, Δlog g = 0.2, Δvt = 0.1 km s-1, Δ[Fe/H] = −0.1 dex. We note that star B3-b1 was chosen for its reanalysis by Ryde et al. (2010), but it has one discardable line that gives a low Mn (in parenthesis) to which a low weight is given since it disagrees with the other three lines, and only an extra − 0.05 dex is added to the mean of the other three lines.

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