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Home All issues Volume 570 (October 2014) A&A, 570 (2014) A76 Online Material
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Issue
A&A
Volume 570, October 2014
Article Number A76
Number of page(s) 21
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361/201424311
Published online 21 October 2014

Online material

Appendix A: Equivalent widths and atomic data

In Table A.1 we list the hyperfine structure constants for the BaII 6141.713 and 6496.897 Å lines, in Table A.2 the list of lines substructured because of the hyperfine structure. In Table A.3 we list the hyperfine structure constants for LaII lines studied in this work.

In Table A.4 we report the lines that blend and overlap Sr i 6503.989, 6550.244 Å, and Y ii 6613.733.

Table A.5 presents the equivalent widths of FeI and FeII lines used in the analysis. In Fig. A.1 we plot the EWs measured in the UVES spectra in 2014 (EW(2014)) vs. EWs measured in the GIRAFFE spectra in 2009 (EW(2009)), and residuals between the two. For star B-108, we also compare the measurements with IRAF on the UVES spectra and with EW(2009). The better de-blending of lines with IRAF from the probable presence of two stars explains the poor fit between IRAF and the other EWs.

Table A.1

Atomic constants for BaII used to compute the hyperfine structure: A constants are taken from Rutten (1978), B constants from Biehl (1976), and when the B constants were not available in the literature we assumed them to be null.

Table A.2

Hyperfine structure for Ba ii lines. log gf adopted: fitting on solar and Arcturus spectra.

Table A.3

Atomic constants for LaII used to compute hyperfine structure: A and B constants are from Lawler et al. (2001a) and Biehl (1976), and where the B constants were not available in the literature, we assumed them as null.

Table A.4

Blends near and overlapping the Sr i 6503.989, 6550.244 Å, and Y ii 6613.733 lines.

Table A.5

Fe i and Fe ii lines employed, their wavelengths, excitation potential (eV), oscillator strengths adopted from B09, and equivalent widths as given in B09 from GIRAFFE spectra, and those we measured with the code DAOSPEC on UVES spectra. For star B-108 we also measured EWs with IRAF.

thumbnail Fig. A.1

Equivalent widths measured in the UVES spectra in 2014 (EW(2014)) vs. equivalent widths measured in the GIRAFFE spectra in 2009 (EW(2009)), and residuals between the two. For each star the upper panel gives EW(2014) vs. EW(2009), and the lower panel gives the residuals. For star B-108, also the measurements with IRAF on the UVES spectra are compared with EW(2009).
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