All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{fig/7217fig1} \end{figure}$ Figure 1: Sketch illustrating the construction of the light cones. A sequence of N lens planes (vertical lines) is used to fill the space between the observer (O) and the sources on the (N+1)-th plane. The aperture of the light cone depends on the distance to the last lens plane. At low redshifts, only a small fraction of the lens planes enters the light-cone (dark-gray shaded region). This fraction increases by reducing the redshift of the sources, increasing the aperture of the light cone (light-gray shaded region).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{fig/7217fig2} \end{figure}$ Figure 2: Number of halos per mass bin per square degree. The red and green curves show the halo mass distribution for sources at $z_{\rm s}=1$ and $z_{\rm s}=2$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{fig/7217fig3CMJN.eps} \end{figure}$ Figure 3: Numerical power spectra of the effective convergence (solid line) and of the shear (dotted line) obtained by averaging over 60 different light cones corresponding to a solid angle of $\sim$ 13 square degrees. The power spectrum expected for a $\Lambda$ CDM model with the same cosmological parameters as the simulation is given by the dashed line. The errorbars are shown only for the effective convergence power spectrum, but are of equivalent size for the shear power spectrum.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{fig/7217fg14} \end{figure}$ Figure 4: Comparison of the different filter shapes used here and in the literature. The filter scales $r_{\rm s}$ are those typically used in the literature. Note how the optimal filter (black solid curve) shrinks when the linear matter power spectrum is used to suppress the LSS contribution (red dashed curve). Interestingly, Hennawi & Spergel (2005) found experimentally that the truncated NFW-shaped filter (cyan curve) performs best when scaled to the green curve (THS), which approximates the optimal filter (OPT, red curve) almost precisely. The advantage of the optimal compared to the other filters is that its shape and scale are physically and statistically well motivated such that it needs not be experimentally rescaled.
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm]{fig/7217fg4a}\hspace*{2mm} \in... ...7217fg4e}\hspace*{2mm} \includegraphics[width=4.4cm]{fig/7217fg4f} \end{figure}$ Figure 5: Maps of the effective convergence for sources at redshift $z_{\rm s}=1$ ( left panels) and $z_{\rm s}=2$ ( right panels) for a region of simulated sky. Superimposed are the iso-contours of the signal-to-noise ratio of the weak-lensing signal measured with three estimators, namely the APT ( top panels), the OAPT ( middle panels) and the OPT ( bottom panels). The iso-contours start from S/N=4 with a step of 3. The positions of the halos contained in the field-of-view having mass $M>7\times 10^{13}~h^{-1}~M_\odot$ are identified by circles. The filter sizes are 11', 20' and 4' for the APT, the OAPT and the OPT, respectively.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=4.4cm,clip]{fig/7217fg5a}\hfill \includegraphics[width=4.4cm,clip]{fig/7217fg5b} }\end{figure}$ Figure 6: Map of the S/N ratio corresponding to a region of 3 square degrees. The map was created using the OAPT estimator, with a filter scale of 20' and assuming a source redshift of $z_{\rm s}=1$ . The left panel shows the S/N ratio map including all lens planes, while the right panel shows the same map obtained after removing the lens plane containing the cluster responsible for the highest S/N peak in the left panel.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=4.4cm,clip]{fig/7217f13a}\hfill \includegraphics[width=4.4cm,clip]{fig/7217f13b} }\end{figure}$ Figure 7: Maps of the S/N ratio corresponding to a region of 3 square degrees. The maps were created with the APT estimator, with a filter scale of 11' and assuming a source redshift of $z_{\rm s}=2$ . The left panel shows a true detection, while the right panel shows a spurious detection.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=4.4cm,angle=-90]{fig/7217fg6a}\... ...e}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217fg6f} }\end{figure}$ Figure 8: Number of detections as a function of the S/N ratio obtained by using the APT ( top panels), the OAPT ( middle panels) and the OPT weak lensing estimators. Results for sources at redshift $z_{\rm s}=1$ and $z_{\rm s}=2$ are shown in the left and in the right panels, respectively. Different line styles refer to three different filter sizes. For the OPT, these are 1', 2' and 4'. They correspond to 2.75', 5.5', and 11' for the APT and to 5', 10' and 20' for the OAPT.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[height=4.4cm,angle=-90]{fig/7217fg7a}... ...e}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217fg7f} }\end{figure}$ Figure 9: Fraction of spurious detections as a function of the S/Nratio obtained by using the APT ( top panels), the OAPT ( middle panels) and the OPT weak-lensing estimators. Results for sources at redshift $z_{\rm s}=1$ and $z_{\rm s}=2$ are shown in the left and the right panels, respectively. Different line styles refer to three filter sizes. For the OPT these are 1', 2' and 4'. They correspond to 2.75', 5.5', and 11' for the APT and to 5', 10' and 20' for the OAPT.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=4.4cm,angle=-90]{fig/7217fg8a}\... ...e}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217fg8f} }\end{figure}$ Figure 10: Minimum detected halo mass as a function of redshift for the APT ( top panels), the OAPT ( middle panels) and for the OPT ( bottom panels) estimators. Results for sources at redshift $z_{\rm s}=1$ and $z_{\rm s}=2$ are shown in the left and in the right panels, respectively. Different line styles refer to three filter sizes. For the OPT, these are 1', 2' and 4'. They correspond to 2.75', 5.5', and 11' for the APT and to 5', 10' and 20' for the OAPT. Results for each redshift bin are averaged between two planes.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=4.4cm,angle=-90]{fig/7217fg9a}\... ...e}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217fg9f} }\end{figure}$ Figure 11: Fraction of detections as a function of the halo mass. Each plot contains results obtained with the three filter radii used in this work. The panels on the left show curves for sources at $z_{\rm s}=1$ , the panels on the right for sources at $z_{\rm s}=2$ . From top to bottom we have the APT, the OAPT and the OPT.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=4.4cm,angle=-90]{fig/7217f12a}\... ...e}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217f12f} }\end{figure}$ Figure 12: Fraction of halo detections with the APT, OAPT and OPT (from top to bottom) as a function of the halo redshift for three particular masses. The red line corresponds to a mass of $M=2.5\times 10^{13} M_{\odot }/h$ , the green line to $M=5\times 10^{13} M_{\odot }/h$ and the blue line to $M=10^{14} M_{\odot }/h$ . The panels on the left show the results for sources at $z_{\rm s}=1$ and those on the right for sources at $z_{\rm s}=2$ . From top to bottom, the filter radii are r=5.5' (for APT), r=10' (for OAPT) and r=2' (for OPT). Results for each redshift bin are averaged between two planes.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[height=4.4cm,angle=-90]{fig/7217f10a}... ...c}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217f10f} }\end{figure}$ Figure 13: Total number of detections per square degree ( left panels) and fraction of spurious detections ( right panels) for sources distributed in redshift as in the GaBoDS survey (Schirmer et al. 2003). From top to bottom, we show the APT (for r=2.75', r=5.5' and r=11'), the OAPT (r=5', r=10' and r=20') and the OPT (r=1', r=2' and r=4').
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{fig/7217fig2} \end{figure}$	Figure 2: Number of halos per mass bin per square degree. The red and green curves show the halo mass distribution for sources at $z_{\rm s}=1$ and $z_{\rm s}=2$ , respectively.
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$\begin{figure} \par\mbox{ \includegraphics[width=4.4cm,clip]{fig/7217f13a}\hfill \includegraphics[width=4.4cm,clip]{fig/7217f13b} }\end{figure}$	Figure 7: Maps of the S/N ratio corresponding to a region of 3 square degrees. The maps were created with the APT estimator, with a filter scale of 11' and assuming a source redshift of $z_{\rm s}=2$ . The left panel shows a true detection, while the right panel shows a spurious detection.
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$\begin{figure} \par\mbox{\includegraphics[height=4.4cm,angle=-90]{fig/7217fg9a}\... ...e}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217fg9f} }\end{figure}$	Figure 11: Fraction of detections as a function of the halo mass. Each plot contains results obtained with the three filter radii used in this work. The panels on the left show curves for sources at $z_{\rm s}=1$ , the panels on the right for sources at $z_{\rm s}=2$ . From top to bottom we have the APT, the OAPT and the OPT.
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$\begin{figure} \par\mbox{ \includegraphics[height=4.4cm,angle=-90]{fig/7217f10a}... ...c}\hfill \includegraphics[height=4.4cm,angle=-90]{fig/7217f10f} }\end{figure}$	Figure 13: Total number of detections per square degree ( left panels) and fraction of spurious detections ( right panels) for sources distributed in redshift as in the GaBoDS survey (Schirmer et al. 2003). From top to bottom, we show the APT (for r=2.75', r=5.5' and r=11'), the OAPT (r=5', r=10' and r=20') and the OPT (r=1', r=2' and r=4').
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