All Figures

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708fig1.eps}\hspace*{6mm} \includegraphics[width=7.9cm,clip]{7708fig2.eps}\end{figure}$ Figure 1: Typical apodizer shape for the bell regime ( left) and the bagel regime ( right). Central obscuration is 30 $\%$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7708fig3.eps}\end{figure}$ Figure 2: Diagram of a coronagraph showing the pupil plane containing the apodizer ( $\psi _{\rm A}$ ), the focal plane with the FPM ( $\psi _{\rm B}$ ), the pupil image spatially filtered by the stop ( $\psi _{\rm C}$ ) and the detector plane ( $\psi _{\rm D}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708fig4.eps}\end{figure}$ Figure 3: Apodizer throughput (relative to full transmission of the telescope pupil) as a function of FPM diameter for different obscuration sizes.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708fig5.eps}\end{figure}$ Figure 4: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of the FPM diameter and obscuration sizes, in the case of the APLC and classical Lyot coronagraph.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{7708fig6.eps}\end{figure}$ Figure 5: Radial profiles of PSFs and coronagraphic images obtained with optimal APLC (using $C_{\mathscr{C}}$ ) for several obscuration sizes.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7708fig7.eps}\end{figure}$ Figure 6: Pupil configurations considered in this paper.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708fig8.eps}\end{figure}$ Figure 7: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of the FPM diameter and number of spider arms. Spider thickness is set to 62 cm.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708fig9.eps}\end{figure}$ Figure 8: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of the FPM diameter and reflectivity variations.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708figa.eps}\end{figure}$ Figure 9: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of the FPM diameter and spider arm thickness. Number of spider arms is set to 6.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708figb.eps}\end{figure}$ Figure 10: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of the FPM diameter and pupil shear.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708figc.eps}\end{figure}$ Figure 11: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of the FPM diameter and low-order aberrations.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7708figd.eps}\end{figure}$ Figure 12: $C_{\mathscr{C}}$ average between 3 and 100 $\lambda /D$ as a function of FPM diameter and the filter bandpass.
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In the text

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{7708fige.eps}\includegraphics[width=4.8cm,clip]{7708figf.eps}\end{figure}$ Figure 13: Optimized apodized E-ELT apertures: telescope design 1 ( left), telescope design 2 ( right).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7708figg.eps}\hspace*{6mm} \includegraphics[width=8cm,clip]{7708figh.eps}\end{figure}$ Figure 14: Radial profiles of PSFs and coronagraphic images ( $\Delta \lambda \slash \lambda = 20\%$ ) for the 2 designs considering throughput optimization ( up) or $C_{\mathscr{C}}$ optimization ( bottom).
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In the text