Free Access
Volume 579, July 2015
Article Number A47
Number of page(s) 18
Section Stellar atmospheres
Published online 25 June 2015

Online material

Appendix A: Appendix A

Appendix A.1: A.1. An alternative approach to determining Vt

In this Appendix we show the standard deviation around the mean abundance plotted as a function of the microturbulent velocity, following the approach of Sahin et al. (2011). The

thumbnail Fig. A.1

Standard deviation around the mean abundances as a function of microturbulence Vt for HQ Car, shown for several elements.

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thumbnail Fig. A.2

Same as Fig. A.1, but for DD Vel.

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dispersion of the abundances is computed for the Fe I, Fe II, Si I, and Ni I lines, while the microturbulent velocity Vt is varied from 1 to 6 km s-1. The minimum value of the dispersion is in good agreement within the different elements, confirming the values of the microturbulence (derived solely from Fe I) adopted in this study, namely 3.1 km s-1 for HQ Car and 3.8 km s-1 for DD Vel.

Appendix A.2: A.2. List of lines used

Table A.1

Atomic parameters and EWs of HQ Car and DD Vel.

Appendix B: Appendix B: Solar references

Table A.1

Solar abundance derived from the solar spectrum using the grid of models by Castelli & Kurucz (2004), compared to the solar photospheric abundance by Asplund et al. (2009) and by Reddy et al. (2003).

© ESO, 2015

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