All Figures

$\begin{figure} \par\includegraphics[angle=-90, width=9cm,clip]{10058f1.eps} \end{figure}$ Figure 1: 7 years of RV measurements for Proxima Cen using UVES+I₂ cell at the ESO VLT. (The secular acceleration has been subtracted.) The data have a total rms of $3.11~{\rm m~s}^{-1}$ and an average uncertainty of $2.34~{\rm m~s}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=8.5cm,clip]{10058f2.eps} \end{figure}$ Figure 2: Lomb-Scargle periodogram of the Proxima Cen RV data. The upper panel shows the power spectrum and the lower panel displays the window function. The 1-year peak in our window function is quite dominant. Using the bootstrap method to estimate the significance of the peak shows that no significant signal, except the peak close to 1 year, is present in our data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=9cm,clip]{10058f3.eps} \end{figure}$ Figure 3: Proxima Cen H $_{\alpha }$ line index measurements as a function of RV. The error bar of the line index is the rms of the individual measurements (within one night) binned to form one data point, in the same manner as the RV data. There appears to be a weak correlation between the H $_{\alpha }$ index and the RV data. The linear correlation coefficient is -0.23. A fit to the data is shown as a dashed line. The residual RV scatter around this slope is $3.03~{\rm m~s}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[origin=rb,angle=-90, width=12cm,clip]{10058f4.eps}\end{figure}$ Figure 4: Mass upper limits for planets in circular orbits around Proxima Cen based on our numerical simulations. All test signals with amplitudes corresponding to masses on and above the solid line were recovered with a >99% significance. The solid, dashed, dashed-dotted and long-dashed lines show the mass range where we successfully recovered 100, 75, 50 and 25% of the test signals. The shaded area labelled ``HZ'' displays the approximate location of the classic liquid water habitable zone (after Kasting et al. 1993). The region labelled ``1-year window'' shows the period range that we excluded from our simulations.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=9cm,clip]{10058f1.eps} \end{figure}$	Figure 1: 7 years of RV measurements for Proxima Cen using UVES+I₂ cell at the ESO VLT. (The secular acceleration has been subtracted.) The data have a total rms of $3.11~{\rm m~s}^{-1}$ and an average uncertainty of $2.34~{\rm m~s}^{-1}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90, width=8.5cm,clip]{10058f2.eps} \end{figure}$	Figure 2: Lomb-Scargle periodogram of the Proxima Cen RV data. The upper panel shows the power spectrum and the lower panel displays the window function. The 1-year peak in our window function is quite dominant. Using the bootstrap method to estimate the significance of the peak shows that no significant signal, except the peak close to 1 year, is present in our data.
Open with DEXTER