All Figures

$\begin{figure} \par\includegraphics[width=5.3cm,clip]{7288fig1.ps}\end{figure}$ Figure 1: Scheme for the use of ARES.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7288fig2.ps}\end{figure}$ Figure 2: A synthetic spectrum region with a signal-to-noise ratio around 50. The filled line represents the fit to the local continuum through a 2nd-order polynomial based on the points that are marked as crosses in the spectrum. We can see the variations induced by some different choises to determine the local continuum (effect of the parameter rejt, cf. Sect. 4.1).
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In the text

$\begin{figure} \par\includegraphics[width=16.1cm,clip]{7288fig3.ps}\end{figure}$ Figure 3: A simulated normalized spectral region and the respective 1st, 2nd, and 3rd derivatives. In the right panel it is easily seen that the local maxima of the 2nd derivative, which can be found using the zeros of the 3rd derivatives, estimates the center of the lines of the simulated spectrum very well. Note that using this we can see extremely blended lines that do not present zeros on the 1st derivative. The left and middle panels show how the parameter smoothder is useful for eliminating the noise when computating the derivatives.
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In the text

$\begin{figure} \par\includegraphics[width=16.1cm,clip]{7288fig4.ps}\end{figure}$ Figure 4: ARES results for different kinds of spectra in terms of resolution and noise contamination. The larger plot shows the comparison between ARES EWs (y axes) and "hand made'' EWs (x axes). In the box we present the slope of the linear fit to the points (dashed line), the rms, the number of identified lines, and the mean difference in the EW of the measurements. The filled line is a 1:1 line. The small plots represent the variations in the values presented on the box for the different spectra. On the left we fixed the resolution and changed the noise levels. On the right we fixed the noise level and changed the resolution. Note that these results can be improved if a more careful choice of the input parameters is made for each spectrum type.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{7288fig5.ps}\end{figure}$ Figure 5: Results of both ARES ( right) and DAOSPEC ( left) comparisons to "hand made'' measurements using the same sample of FEROS spectra. The dotted histogram represents the lines that are weaker than 40 mÅ. The thin line histogram represents the lines that are stronger than 40 mÅ.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7288fig6.ps}\end{figure}$ Figure 6: Results of ARES for a sample of HARPS spectra comparing the value of the EW obtained by ARES ( $EW_{\rm ARES}$ ) with the "manual'' value from IRAF ( $EW_{\rm IRAF}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7288fig7.ps}\end{figure}$ Figure 7: Results of ARES for a sample of UVES spectra comparing the value of the EW obtained by ARES ( $EW_{\rm ARES}$ ) with the "manual'' value from IRAF ( $EW_{\rm IRAF}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{7288fig8.ps}\end{figure}$ Figure 8: Comparison of the manual obtained spectroscopic parameters to the obtained automatically through ARES code.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{7288fig9.ps}\end{figure}$ Figure 9: Results for the fit of the abundances for determining the stellar parameters for the FEROS spectra of HD20201. The crosses represent the Fe I, and the filled triangles the Fe II.
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In the text

$\begin{figure} \par\includegraphics[width=5.3cm,clip]{7288fig1.ps}\end{figure}$	Figure 1: Scheme for the use of ARES.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{7288fig2.ps}\end{figure}$	Figure 2: A synthetic spectrum region with a signal-to-noise ratio around 50. The filled line represents the fit to the local continuum through a 2nd-order polynomial based on the points that are marked as crosses in the spectrum. We can see the variations induced by some different choises to determine the local continuum (effect of the parameter rejt, cf. Sect. 4.1).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{7288fig5.ps}\end{figure}$	Figure 5: Results of both ARES ( right) and DAOSPEC ( left) comparisons to "hand made'' measurements using the same sample of FEROS spectra. The dotted histogram represents the lines that are weaker than 40 mÅ. The thin line histogram represents the lines that are stronger than 40 mÅ.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7288fig6.ps}\end{figure}$	Figure 6: Results of ARES for a sample of HARPS spectra comparing the value of the EW obtained by ARES ( $EW_{\rm ARES}$ ) with the "manual'' value from IRAF ( $EW_{\rm IRAF}$ ).
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7288fig7.ps}\end{figure}$	Figure 7: Results of ARES for a sample of UVES spectra comparing the value of the EW obtained by ARES ( $EW_{\rm ARES}$ ) with the "manual'' value from IRAF ( $EW_{\rm IRAF}$ ).
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{7288fig8.ps}\end{figure}$	Figure 8: Comparison of the manual obtained spectroscopic parameters to the obtained automatically through ARES code.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{7288fig9.ps}\end{figure}$	Figure 9: Results for the fit of the abundances for determining the stellar parameters for the FEROS spectra of HD20201. The crosses represent the Fe I, and the filled triangles the Fe II.
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