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
Central wavelengths and total literature and adopted oscillator strengths.
Hyperfine structure for Mn i lines.
Uncertainties on derived [Mn/Fe] for the metal-poor star B3-b1 and the red clump star BWc-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.
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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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Fig. 2
Fits of the four Mn i lines for the metal-poor ([Fe/H] = −0.47) star BL-7. |
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Fig. 3
Fits of the four Mn i lines for the metal-poor ([Fe/H] = −1.21) star BW-f4. |
Open with DEXTER |
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Fig. 4
Fits of the four Mn i lines for the most metal-poor ([Fe/H] = −1.27) sample star BW-f8. |
Open with DEXTER |
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Fig. 5
Fits of the four Mn i lines for the metal-poor ([Fe/H] = −0.78) star B3-b1. |
Open with DEXTER |
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Fig. 6
Fits of the four Mn i lines for the ([Fe/H] = −0.25) red clump star BWc-7. |
Open with DEXTER |
© ESO, 2013
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