Astronomy & Astrophysics

All Figures

$\begin{figure} \par\epsfig{file=2334fig1.ps,width=8.3cm,clip}\end{figure}$ Figure 1: Example of an instrumental light curve before ( top) and after the partial correction of scattered light (once underestimated ( middle), and once overestimated ( bottom)). The sharp peaks in the upper plot are due to the SAA crossing; they become gaps in the output light curves.
Open with DEXTER

In the text

$\begin{figure} \par\epsfig{file=2334fig2.ps,width=8cm,clip} \end{figure}$ Figure 2: A) and B) are two correlation functions ("detection curves'' DC) showing systematic noise. Artefacts are sometimes obvious (synchroneous spikes and similar envelope) or can be hidden, with a known or unknown origin. C) and D) show DC613 before then after detrending (note the very different y-axis scales).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.5cm,clip]{2334fig3.eps} \end{figure}$ Figure 3: The different steps of the light curve analysis of Team 2 for light curve ID34. First the data gaps (not visible at this scale) are interpolated and the light curve is normalized ( top), and a lowpass-filter is applied to remove high frequency signals ( middle). Finally the stellar variability is modeled and a search for period signals performed ( bottom). The periodic signal found is marked in the figure.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics{2334fig4.eps}}\vspace*{0.5mm} \par\resizebox{8.5cm}{!}{\includegraphics{2334fig5.eps}}\end{figure}$ Figure 4: Top: The adjusted SR function for light curve 34, which shows the typical peaks of a transit signal. Bottom: The distribution of the normalized SR of the 999 light curves. The arrow points to the adopted detection threshold of 7.0 (Team 3).
Open with DEXTER

In the text

$\begin{figure} \par\epsfig{file=2334fig6.eps,width=7.8cm,clip} \end{figure}$ Figure 5: Light curve 34 before ( top) and after ( bottom) iterative non-linear filtering with a trial duration of 3.3 h (Team 5). The Y-axis represents a relative flux.
Open with DEXTER

In the text

$\begin{figure} \par\epsfig{file=2334fig7.eps,width=8cm,clip} \end{figure}$ Figure 6: Candidate selection in the multiple ( $S_{\rm M}$ ) versus single ( $S_{\rm S}$ ) transit detection statistic plane (trial duration 3.3 h). Solid line: detection threshold. Dashed line: low-confidence threshold. Diamonds: correct detections. Squares: false detections (grey: excluded at the light curve examination stage). Triangles: missed detections (grey: detected using another trial duration). (Team 5)
Open with DEXTER

In the text

$\begin{figure} \par\epsfig{file=2334fig8.ps,width=8.2cm,clip} \end{figure}$ Figure 7: Depth of the transits versus number of transits. Plus signs show the non-detected events, diamonds show the events detected by five groups independently, and filled circles correspond to 1 to 4 detection occurences. The dashed line thus shows the border of the simulated CoRoT detection limit (proportional to n^-1/2). The only plus sign above the detection line is a grazing planet on a faint fluctuating star.
Open with DEXTER

In the text

$\begin{figure} \par\epsfig{file=2334fig1.ps,width=8.3cm,clip}\end{figure}$	Figure 1: Example of an instrumental light curve before ( top) and after the partial correction of scattered light (once underestimated ( middle), and once overestimated ( bottom)). The sharp peaks in the upper plot are due to the SAA crossing; they become gaps in the output light curves.
Open with DEXTER

$\begin{figure} \par\epsfig{file=2334fig2.ps,width=8cm,clip} \end{figure}$	Figure 2: A) and B) are two correlation functions ("detection curves'' DC) showing systematic noise. Artefacts are sometimes obvious (synchroneous spikes and similar envelope) or can be hidden, with a known or unknown origin. C) and D) show DC613 before then after detrending (note the very different y-axis scales).
Open with DEXTER

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics{2334fig4.eps}}\vspace*{0.5mm} \par\resizebox{8.5cm}{!}{\includegraphics{2334fig5.eps}}\end{figure}$	Figure 4: Top: The adjusted SR function for light curve 34, which shows the typical peaks of a transit signal. Bottom: The distribution of the normalized SR of the 999 light curves. The arrow points to the adopted detection threshold of 7.0 (Team 3).
Open with DEXTER

$\begin{figure} \par\epsfig{file=2334fig6.eps,width=7.8cm,clip} \end{figure}$	Figure 5: Light curve 34 before ( top) and after ( bottom) iterative non-linear filtering with a trial duration of 3.3 h (Team 5). The Y-axis represents a relative flux.
Open with DEXTER