All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f1.eps}\end{figure}$ Figure 1: From top to bottom: a small section of the co-added OGLE-TR-3 spectrum and the individual spectra of the ten observing blocks (1 h observing time each) ordered by JD as listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.8cm,clip]{4189f2.eps}\end{figure}$ Figure 2: Three normalized VLT-UVES spectra of OGLE-TR-3, obtained at JD-2452400 = 62.61590, 86.57832, and 89.56877 (from bottom to top), around the NaD doublet. The fit consists of three components: A synthetic spectrum shifted by the measured radial velocity (blue wing), a Gaussian emission component from the earth's atmosphere, and an interstellar absorption of a column density of $5\times 10^{15}$ cm^-2 neutral Na atoms for the red wing. The velocity of the interstellar component has a fixed offset of +20 km s^-1 relative to the stellar component.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f3.eps}\end{figure}$ Figure 3: Co-added differences between red "+'' and blue "*'' wings of observed spectral lines and Gauss profiles with 1 $\sigma$ error bars. The spectra from JD = 86.53247 and 86.57832 are omitted due to very large uncertainties. No indication of line asymmetry is present in our data set.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.4cm,clip]{4189f4.eps}\end{figure}$ Figure 4: Four 50 Å sections of the co-added spectrum of OGLE-TR-3 compared to a theoretical model: $T_{\rm eff}=6100~$ K, $\log g =4.5$ (cgs), and sub-solar abundances ( $[{\rm M/H}]=-0.5$ ).
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{4189f5.eps}\end{figure}$ Figure 5: The parameters of OGLE-TR-3 compared to stellar evolution models (Schaerer et al. 1993). The evolution tracks as well as the lines of constant radii are labeled in solar units.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4189f6.eps}\end{figure}$ Figure 6: An example of the cross-correlation. Co-added spectrum versus the one from JD = 2452486.53247 in the interval [5350 Å-5400 Å] (++++) and a Gauss fit (solid line).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4189f7.eps}\end{figure}$ Figure 7: Measurements of the radial velocity of OGLE-TR-3. Error bars indicate 1 $\sigma$ deviations. The solid line is the best fit from our $\chi ^2$ -minimization, the dashed lines are the 3 $\sigma$ deviations of the amplitude.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4189f8.eps}\end{figure}$ Figure 8: Measurements of the velocity shift of the night sky emission lines in the spectra of OGLE-TR-3. Error bars indicate 1 $\sigma$ deviations. The solid line is the best fit from our $\chi ^2$ -minimization.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{4189f9.eps}\end{figure}$ Figure 9: Fit results of synthetic white noise curves versus fit results of the OGLE-TR-3 radial velocity (RV) curve using pikaia. While the synthetic data (ordinate) spread over a wide interval, the real data (abscissa) are confined to a narrow range only. The ratio between the distribution widths of the fits is indicated in the plots.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f10.eps}\end{figure}$ Figure 10: Light curve of OGLE-TR-3 from Udalski et al. (2002a): top and middle: I band observed (++++) and synthetic light curve (solid line). Bottom: predicted H band light curve at a smaller scale. The primary eclipse is shown in the top panel, the secondary eclipse in the lower two.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f11.eps}\end{figure}$ Figure 11: Light curve of OGLE-TR-3 from Udalski et al. (2002a): I band observed (++++) and synthetic light curve (solid line). The photometric data are folded with 2 $\times$ 1.1899 days in order to simulate the G+[M+M] scenario. The eclipsing system (primary minimum top, secondary minimum bottom panel) consists of two M2 stars; the third light contribution is that from a G star.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f12.eps}\end{figure}$ Figure 12: Predicted eclipse durations for blending scenarios as function of the spectral type of the secondary (first to fourth contact: full line; second to third contact dashed line) in units of eclipse durations of OGLE-TR-3. Contribution from a foreground star with 70, 80, 90, 95, 98% is labeled with crosses, stars, squares, diamonds, and triangles respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f1.eps}\end{figure}$	Figure 1: From top to bottom: a small section of the co-added OGLE-TR-3 spectrum and the individual spectra of the ten observing blocks (1 h observing time each) ordered by JD as listed in Table 1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f3.eps}\end{figure}$	Figure 3: Co-added differences between red "+'' and blue "*'' wings of observed spectral lines and Gauss profiles with 1 $\sigma$ error bars. The spectra from JD = 86.53247 and 86.57832 are omitted due to very large uncertainties. No indication of line asymmetry is present in our data set.
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$\begin{figure} \par\includegraphics[angle=90,width=17.4cm,clip]{4189f4.eps}\end{figure}$	Figure 4: Four 50 Å sections of the co-added spectrum of OGLE-TR-3 compared to a theoretical model: $T_{\rm eff}=6100~$ K, $\log g =4.5$ (cgs), and sub-solar abundances ( $[{\rm M/H}]=-0.5$ ).
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$\begin{figure} \par\includegraphics[width=15cm,clip]{4189f5.eps}\end{figure}$	Figure 5: The parameters of OGLE-TR-3 compared to stellar evolution models (Schaerer et al. 1993). The evolution tracks as well as the lines of constant radii are labeled in solar units.
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4189f6.eps}\end{figure}$	Figure 6: An example of the cross-correlation. Co-added spectrum versus the one from JD = 2452486.53247 in the interval [5350 Å-5400 Å] (++++) and a Gauss fit (solid line).
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4189f7.eps}\end{figure}$	Figure 7: Measurements of the radial velocity of OGLE-TR-3. Error bars indicate 1 $\sigma$ deviations. The solid line is the best fit from our $\chi ^2$ -minimization, the dashed lines are the 3 $\sigma$ deviations of the amplitude.
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{4189f8.eps}\end{figure}$	Figure 8: Measurements of the velocity shift of the night sky emission lines in the spectra of OGLE-TR-3. Error bars indicate 1 $\sigma$ deviations. The solid line is the best fit from our $\chi ^2$ -minimization.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{4189f9.eps}\end{figure}$	Figure 9: Fit results of synthetic white noise curves versus fit results of the OGLE-TR-3 radial velocity (RV) curve using `pikaia`. While the synthetic data (ordinate) spread over a wide interval, the real data (abscissa) are confined to a narrow range only. The ratio between the distribution widths of the fits is indicated in the plots.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f10.eps}\end{figure}$	Figure 10: Light curve of OGLE-TR-3 from Udalski et al. (2002a): top and middle: I band observed (++++) and synthetic light curve (solid line). Bottom: predicted H band light curve at a smaller scale. The primary eclipse is shown in the top panel, the secondary eclipse in the lower two.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f11.eps}\end{figure}$	Figure 11: Light curve of OGLE-TR-3 from Udalski et al. (2002a): I band observed (++++) and synthetic light curve (solid line). The photometric data are folded with 2 $\times$ 1.1899 days in order to simulate the G+[M+M] scenario. The eclipsing system (primary minimum top, secondary minimum bottom panel) consists of two M2 stars; the third light contribution is that from a G star.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4189f12.eps}\end{figure}$	Figure 12: Predicted eclipse durations for blending scenarios as function of the spectral type of the secondary (first to fourth contact: full line; second to third contact dashed line) in units of eclipse durations of OGLE-TR-3. Contribution from a foreground star with 70, 80, 90, 95, 98% is labeled with crosses, stars, squares, diamonds, and triangles respectively.
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