Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H3937F1.eps} \end{figure}$ Figure 1: Distribution of dwarfs in the 3.5 deg²synthesized field vs. the visual magnitude. Dashed line: complete Besançon model (16 000 stars for $V \le 16.5$ ). Solid line: selection of the 12 000 brightest targets for COROT.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H3937F2.eps} \end{figure}$ Figure 2: Same as Fig. 1 vs. the spectral type.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H3937F3.eps} \end{figure}$ Figure 3: Number of expected detections for the entire mission as a function of the reduced orbital distance for various planetary radii (expressed in unit of the Earth radius). It is assumed that every star has one planet of the labelled radius positioned at the considered distance.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{H3937F4.eps} \end{figure}$ Figure 4: Number of expected detections for the entire mission as a function of the planet effective temperature for various planetary radii (expressed in unit of the Earth radius). It is assumed that every star has one planet of the labelled radius with the considered effective temperature.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{H3937F5.eps} \end{figure}$ Figure 5: Histograms of expected detections for the whole mission - with a false alarm rate less than one false detection - vs. the parent star spectral type, for various planetary radii (expressed in unit of the Earth radius). The planets are assumed to be uniformly distributed as a function of their reduced orbital distances. The crowding effect (Sect. 5.2) is expected to remove $\approx$ $10\%$ from the detections plotted here.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{H3937F6.eps} \end{figure}$ Figure 6: Same as Fig. 5 vs. the visual magnitude of the parent star.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H3937F7.eps} \end{figure}$ Figure 7: Fraction of a background star flux included in a target mask vs. the distance between their photocenters, once averaged over all relative orientations.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H3937F1.eps} \end{figure}$	Figure 1: Distribution of dwarfs in the 3.5 deg²synthesized field vs. the visual magnitude. Dashed line: complete Besançon model (16 000 stars for $V \le 16.5$ ). Solid line: selection of the 12 000 brightest targets for COROT.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H3937F2.eps} \end{figure}$	Figure 2: Same as Fig. 1 vs. the spectral type.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H3937F3.eps} \end{figure}$	Figure 3: Number of expected detections for the entire mission as a function of the reduced orbital distance for various planetary radii (expressed in unit of the Earth radius). It is assumed that every star has one planet of the labelled radius positioned at the considered distance.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{H3937F4.eps} \end{figure}$	Figure 4: Number of expected detections for the entire mission as a function of the planet effective temperature for various planetary radii (expressed in unit of the Earth radius). It is assumed that every star has one planet of the labelled radius with the considered effective temperature.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{H3937F6.eps} \end{figure}$	Figure 6: Same as Fig. 5 vs. the visual magnitude of the parent star.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H3937F7.eps} \end{figure}$	Figure 7: Fraction of a background star flux included in a target mask vs. the distance between their photocenters, once averaged over all relative orientations.
Open with DEXTER