Age and metallicity of star clusters in the Small Magellanic Cloud from integrated spectroscopy

B. Dias; P. Coelho; B. Barbuy; L. Kerber; T. Idiart

doi:10.1051/0004-6361/200912894

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Volume 520 (September-October 2010)

A&A, 520 (2010) A85

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Issue		A&A Volume 520, September-October 2010


Article Number		A85
Number of page(s)		17
Section		Stellar atmospheres
DOI		https://doi.org/10.1051/0004-6361/200912894
Published online		07 October 2010

Online Material

Appendix A: Spectral fits

$\begin{figure} \begin{flushleft} In this section, the best fits are shown for ea... ...}\vspace*{3mm} \par\includegraphics[width=8.8cm,clip]{12894fgA1.ps} \end{figure}$	Figure A.1: Upper panel: observed spectrum (black line) for the cluster HW1 and the best model fitted by S TARLIGHT+PEGASE-HR (blue line). Lower panel: residuals of the fit.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA2.ps} \end{figure}$	Figure A.2: Same as Fig. A.1 for cluster K3 (ESO).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA3.ps} \end{figure}$	Figure A.3: Same as Fig. A.1 for cluster K3 (LNA).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA4.ps} \end{figure}$	Figure A.4: Same as Fig. A.1 for cluster L3.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA5.ps} \end{figure}$	Figure A.5: Same as Fig. A.1 for cluster L11.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA6.ps} \end{figure}$	Figure A.6: Same as Fig. A.1 for cluster L113.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA7.ps} \end{figure}$	Figure A.7: Same as Fig. A.1 for cluster NGC 121 (ESO).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA8.ps} \end{figure}$	Figure A.8: Same as Fig. A.1 for NGC 121 (LNA).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA9.ps} \end{figure}$	Figure A.9: Same as Fig. A.1 for cluster NGC 152.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA10.ps} \end{figure}$	Figure A.10: Same as Fig. A.1 for cluster NGC 222.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA11.ps} \end{figure}$	Figure A.11: Same as Fig. A.1 for cluster NGC 256.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA12.ps} \end{figure}$	Figure A.12: Same as Fig. A.1 for cluster NGC 269.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA13.ps} \end{figure}$	Figure A.13: Same as Fig. A.1 for cluster NGC 294.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA14.ps} \end{figure}$	Figure A.14: Same as Fig. A.1 for cluster NGC 361 (ESO99).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA15.ps} \end{figure}$	Figure A.15: Same as Fig. A.1 for NGC 361 (ESO00).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA16.ps} \end{figure}$	Figure A.16: Same as Fig. A.1 for cluster NGC 419.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA17.ps} \end{figure}$	Figure A.17: Same as Fig. A.1 for cluster NGC 458.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA18.ps} \end{figure}$	Figure A.18: Upper panel: observed spectrum (black line) for the cluster HW1 and the best model fitted by ULySS+PEGASE-HR (blue line). Red pixels correspond to regions of telluric lines and were rejected from the fit. Lower panel: residuals of the fit. The continuous green lines mark the 1- $\sigma$ deviation.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA19.ps} \end{figure}$	Figure A.19: Same as Fig. A.18 for cluster K3 (ESO).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA20.ps} \end{figure}$	Figure A.20: Same as Fig. A.18 for cluster K3 (LNA).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA21.ps} \end{figure}$	Figure A.21: Same as Fig. A.18 for cluster L3.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA22.ps} \end{figure}$	Figure A.22: Same as Fig. A.18 for cluster L11.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA23.ps} \end{figure}$	Figure A.23: Same as Fig. A.18 for cluster L113.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA24.ps} \end{figure}$	Figure A.24: Same as Fig. A.18 for cluster NGC 121 (ESO).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA25.ps} \end{figure}$	Figure A.25: Same as Fig. A.18 for NGC 121 (LNA).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA26.ps} \end{figure}$	Figure A.26: Same as Fig. A.18 for cluster NGC 152.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA27.ps} \end{figure}$	Figure A.27: Same as Fig. A.18 for cluster NGC 222.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA28.ps} \end{figure}$	Figure A.28: Same as Fig. A.18 for cluster NGC 256.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA29.ps} \end{figure}$	Figure A.29: Same as Fig. A.18 for cluster NGC 269.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA30.ps} \end{figure}$	Figure A.30: Same as Fig. A.18 for cluster NGC 294.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA31.ps} \end{figure}$	Figure A.31: Same as Fig. A.18 for cluster NGC 361 (ESO99).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA32.ps} \end{figure}$	Figure A.32: Same as Fig. A.18 for NGC 361 (ESO00).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA33.ps} \end{figure}$	Figure A.33: Same as Fig. A.18 for cluster NGC 419.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{12894fgA34.ps} \end{figure}$	Figure A.34: Same as Fig. A.18 for cluster NGC 458.
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