EDP Sciences
Free Access
Issue
A&A
Volume 559, November 2013
Article Number A5
Number of page(s) 14
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361/201322380
Published online 28 October 2013

Online material

Table 1

Atomic constants used to compute hyperfine structure from Handrich et al. (1969), Biehl (1976), and Brodzinski et al. (1987).

Table 2

Central wavelengths and total literature and adopted oscillator strengths.

Table 3

Hyperfine structure for Mn i lines.

Table 4

Atmospheric parameters adopted from Zoccali et al. (2006) and Lecureur et al. (2007) for the red giants, and from Hill et al. (2011) for the red clump stars, and abundances of [Mn/Fe] derived in the present work.

Table 5

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

Table 6

Uncertainties on the derived [Mn/Fe] value for model changes of ΔTeff = −150 K, Δlog g = 0.2, Δvt = 0.1 km s-1, Δ[Fe/H] = − 0.1 dex, and corresponding total error.

thumbnail Fig. 1

Lines of Mn i fittings on the solar spectrum observed with the UVES spectrograph, and on the Arcturus spectrum (Hinkle et al. 2000). Observed spectrum (dashed lines); synthetic spectra (solid red line).

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thumbnail Fig. 2

Fits of the four Mn i lines for the metal-poor ([Fe/H] = −0.47) star BL-7.

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thumbnail Fig. 3

Fits of the four Mn i lines for the metal-poor ([Fe/H] = −1.21) star BW-f4.

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thumbnail Fig. 4

Fits of the four Mn i lines for the most metal-poor ([Fe/H] = −1.27) sample star BW-f8.

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thumbnail Fig. 5

Fits of the four Mn i lines for the metal-poor ([Fe/H] = −0.78) star B3-b1.

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thumbnail Fig. 6

Fits of the four Mn i lines for the ([Fe/H] = −0.25) red clump star BWc-7.

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© ESO, 2013

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