The ability of intermediate-band Strömgren photometry to correctly identify dwarf, subgiant, and giant stars and provide stellar metallicities and surface gravities

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Volume 521 (October 2010)

A&A, 521 (2010) A40

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Issue		A&A Volume 521, October 2010


Article Number		A40
Number of page(s)		34
Section		Stellar structure and evolution
DOI		https://doi.org/10.1051/0004-6361/200913544
Published online		19 October 2010

Online Material

Appendix A: Stellar sequences

$\begin{figure} \par\vspace*{3mm} \par\includegraphics[width=12cm,clip]{13544fg30.eps} \end{figure}$	Figure A.1: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = 0.50 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg31.eps} \end{figure}$	Figure A.2: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = 0.40 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg32.eps} \end{figure}$	Figure A.3: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = 0.30 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg33.eps} \end{figure}$	Figure A.4: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = 0.20 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg34.eps} \end{figure}$	Figure A.5: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = 0.10 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg35.eps} \end{figure}$	Figure A.6: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = 0.00 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg36.eps} \end{figure}$	Figure A.7: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.10 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg37.eps} \end{figure}$	Figure A.8: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.20 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg38.eps} \end{figure}$	Figure A.9: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.30 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg39.eps} \end{figure}$	Figure A.10: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.40 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg40.eps} \end{figure}$	Figure A.11: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.50 $\pm$ 0.05 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg41.eps} \end{figure}$	Figure A.12: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.60 $\pm$ 0.10 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg42.eps} \end{figure}$	Figure A.13: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -0.80 $\pm$ 0.10 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{13544fg43.eps} \end{figure}$	Figure A.14: The figure shows how the dwarf star sequence was traced from nearby dwarf stars with [Fe/H] = -1.00 $\pm$ 0.20 plotted in the c_1,0 vs. (b-y)₀ diagram.
Open with DEXTER

Appendix B: Table containing the data collected to test calibrations of [Fe/H] in section

How the catalogue is constructed is explained in detail in Sect. 3.

Column 1 lists the Hipparcos number of the star and Col. 2 gives an alternative stellar name. Column 3 gives the photometry reference (SN88 for Schuster & Nissen 1988; O84 for Olsen 1984; O93 for Olsen 1993; and O94 for Olsen 1994a) and Columns 4 to 7 give the uvby photometry. Column 8 gives the colour excess of the star. Columns 9 to 12 give the dereddened uvby photometry. Column 13 and 14 give the average [Fe/H] (on the Valenti & Fischer 2005, scale) and the full range of [Fe/H] (on the same scale as in Col. 13) if the star was found in more than one study. Columns 15 and 16 give the number of references for the [Fe/H] and lists them (1: Valenti & Fischer 2005; 2: Favata et al. 1997; 3: Feltzing & Gustafsson 1998; 4: Chen et al. 2000; 5: Thorén & Feltzing 2000; 6: Santos et al. 2001; 7: Heiter & Luck 2003; Yong & Lambert 2003; 9: Mishenina et al. 2004; 10: Santos et al. 2004; 11: Bonfils et al. 2005; 12: Luck & Heiter 2005; 13: Santos et al. 2005; 14: Woolf & Wallerstein 2005; and 15: Sousa et al. 2006).

Table B.1 is also available the CDS.

Table B.1: Dwarf stars with both Strömgren photometry and [Fe/H] based on high resolution, high S/N spectroscopy.

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