All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,height=6.1cm,clip]{4479F1.ps} \end{figure}$ Figure 1: Magnitude distribution of galaxies in the three fields in the rband. More detailed galaxy count plots, for each filter and for each Deep field, are available on the web at http://terapix.iap.fr/article.php?id_article=382.
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In the text

$\begin{figure} \par\includegraphics[width=4.9cm,height=4.8cm,clip]{4479F2.ps}\in... ...cm]{4479F3.ps}\includegraphics[width=4.9cm,height=4.8cm]{4479F4.ps} \end{figure}$ Figure 2: The mean ellipticity of the stars shows the behavior of the PSF anisotropy for the three fields D1, D3 and D4. For all of the three fields, $\langle e\rangle$ is few percent in the central part and it becomes about $10\%$ in the corners (see also Fig. 3).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,height=7.2cm,clip]{4479F5.ps} \end{figure}$ Figure 3: Bottom panels show the mean tangential ( left panel) and radial ( right panel) uncorrected stellar ellipticity as a function of the distance to the center of the camera for D1rT001 (filled triangles), D3rT001 (filled squares) and D4rT001 (filled circles) fields. Top panels show the same quantities after PSF correction.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,height=5.8cm,clip]{4479F6.ps} \end{figure}$ Figure 4: E-modes (red filled circles) and B-modes (black open circles) top-hat two point statistics of corrected stars show the smallness of residual PSF systematics.
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In the text

$\begin{figure} \par\includegraphics[width=5.9cm,height=11cm,clip]{4479F7.ps} \end{figure}$ Figure 5: Two-point signal statistics (red filled circles): top-hat ( bottom) and $M_{\rm ap}$ ( middle) correlation function ( top), compared with residual systematics (black open circles). Signal error bars are statistical ones.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,height=5.7cm,clip]{4479F8.ps} \end{figure}$ Figure 6: Top-hat variance of the E-modes in the i'-band (red filled circles) and in the r'-band (red filled triangles) for the same data set. Top-hat variance B-modes in the i'-band (black open circles) and in r'-band (black open triangles).
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In the text

$\begin{figure} \par\includegraphics[width=5.9cm,height=11cm,clip]{4479F9.ps} \end{figure}$ Figure 7: Two-point statistics for all the three fields combined. Red filled circles show E-modes, black open circles show B-modes. E-mode error bars include the statistical error and the cosmic variance contribution, while B-modes are affected only by statistical error.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,height=6.2cm,clip]{4479F10.ps} \end{figure}$ Figure 8: Density of galaxies of D1 field as a function of photometric redshift.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,height=5.6cm,clip]{4479F11.ps} \end{figure}$ Figure 9: Top-hat variance for "high-z'' subsample (red filled triangles) and "low-z'' subsample'' (red filled circles). B-modes for the two subsamples are also shown. Error bars include statistical noise and cosmic variance. The data are compared with theoretical fiducial model ( $\Omega _{\rm m}=0.3$ , $\Omega _\Lambda =0.7$ , $\sigma _8=0.88$ and h=0.7) and source distribution n(z) modeled by Eq. (13), with $\alpha =1.98$ , $\beta =0.66$ and $z_{\rm s}=0.0981$ . The low-z source selection is simulated using n(z) between 0.3 < z < 1.2 and zero otherwise (bottom line). Likewise, the red filled triangles and the black open triangles are the E- and B-modes of the "high-z'' sample. The data are compared with the same theoretical model with a high-z source selection simulated using n(z) between z > 0.8 and zero otherwise. Shaded areas show models within $z_{\rm s}=0.0981^{+0.013}_{-0.011}$ that represent the $1 \sigma$ error region on $z_{\rm s}$ as derived from the likelihood parameter estimation.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,height=6.1cm,clip]{4479F12.ps} \end{figure}$ Figure 10: Plot of mean weight per galaxy as a function of magnitude 21.5< r'_AB < 25.5.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=6.1cm,clip]{4479F13.ps} \end{figure}$ Figure 11: The histogram shows the photometric redshift distribution of 21.5< r'_AB < 25.5 galaxies of Hubble Deep Field North and South used in this work. The central solid line is the best fit model. The solid line histogram is that magnitude weighted redshift distribution. The dashed-dot histogram shows the redshift distribution if the galaxies were not magnitude weighted.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=5.6cm,clip]{4479F14.ps} \end{figure}$ Figure 12: $\Omega _{\rm m}$ and $\sigma _8$ constraints with the Deep data only. The contours show 0.68, 0.95 and 0.999 confidence regions. Errors include statistical, covariance and residual systematic contributions. The models are pure Cold Dark Matter fit to the data, marginalized over the redshift distribution (see Sect. 7.2 for the details).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=5.6cm,clip]{4479F15.ps} \end{figure}$ Figure 13: Same as Fig. 12, combined with the CFHTLS Wide data (Hoekstra et al. 2005). For $\Omega _{\rm m}=0.3$ we have $\sigma _8=0.86\pm 0.05$ at $1 \sigma$ (see Sect. 7.2 for details of the error calculation).
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,height=5.6cm,clip]{4479F16.ps} \end{figure}$ Figure 14: Dark energy constraints from the Deep data only. Hidden parameters are marginalized using a flat prior over $\sigma _8\in [0.7,1.0]$ , $h\in [0.6,0.8]$ and within the $\pm 2\sigma$ boundaries of the redshift parameter $z_{\rm s}$ (see Sect. 7.2).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,height=6.1cm,clip]{4479F1.ps} \end{figure}$	Figure 1: Magnitude distribution of galaxies in the three fields in the rband. More detailed galaxy count plots, for each filter and for each Deep field, are available on the web at http://terapix.iap.fr/article.php?id_article=382.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=4.9cm,height=4.8cm,clip]{4479F2.ps}\in... ...cm]{4479F3.ps}\includegraphics[width=4.9cm,height=4.8cm]{4479F4.ps} \end{figure}$	Figure 2: The mean ellipticity of the stars shows the behavior of the PSF anisotropy for the three fields D1, D3 and D4. For all of the three fields, $\langle e\rangle$ is few percent in the central part and it becomes about $10\%$ in the corners (see also Fig. 3).
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$\begin{figure} \par\includegraphics[width=8.7cm,height=7.2cm,clip]{4479F5.ps} \end{figure}$	Figure 3: Bottom panels show the mean tangential ( left panel) and radial ( right panel) uncorrected stellar ellipticity as a function of the distance to the center of the camera for D1rT001 (filled triangles), D3rT001 (filled squares) and D4rT001 (filled circles) fields. Top panels show the same quantities after PSF correction.
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$\begin{figure} \par\includegraphics[width=7.9cm,height=5.8cm,clip]{4479F6.ps} \end{figure}$	Figure 4: E-modes (red filled circles) and B-modes (black open circles) top-hat two point statistics of corrected stars show the smallness of residual PSF systematics.
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$\begin{figure} \par\includegraphics[width=5.9cm,height=11cm,clip]{4479F7.ps} \end{figure}$	Figure 5: Two-point signal statistics (red filled circles): top-hat ( bottom) and $M_{\rm ap}$ ( middle) correlation function ( top), compared with residual systematics (black open circles). Signal error bars are statistical ones.
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$\begin{figure} \par\includegraphics[width=7.4cm,height=5.7cm,clip]{4479F8.ps} \end{figure}$	Figure 6: Top-hat variance of the E-modes in the i'-band (red filled circles) and in the r'-band (red filled triangles) for the same data set. Top-hat variance B-modes in the i'-band (black open circles) and in r'-band (black open triangles).
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$\begin{figure} \par\includegraphics[width=5.9cm,height=11cm,clip]{4479F9.ps} \end{figure}$	Figure 7: Two-point statistics for all the three fields combined. Red filled circles show E-modes, black open circles show B-modes. E-mode error bars include the statistical error and the cosmic variance contribution, while B-modes are affected only by statistical error.
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$\begin{figure} \par\includegraphics[width=8.1cm,height=6.2cm,clip]{4479F10.ps} \end{figure}$	Figure 8: Density of galaxies of D1 field as a function of photometric redshift.
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$\begin{figure} \par\includegraphics[width=7.8cm,height=6.1cm,clip]{4479F12.ps} \end{figure}$	Figure 10: Plot of mean weight per galaxy as a function of magnitude 21.5< r'_AB < 25.5.
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$\begin{figure} \par\includegraphics[width=8cm,height=6.1cm,clip]{4479F13.ps} \end{figure}$	Figure 11: The histogram shows the photometric redshift distribution of 21.5< r'_AB < 25.5 galaxies of Hubble Deep Field North and South used in this work. The central solid line is the best fit model. The solid line histogram is that magnitude weighted redshift distribution. The dashed-dot histogram shows the redshift distribution if the galaxies were not magnitude weighted.
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$\begin{figure} \par\includegraphics[width=6.8cm,height=5.6cm,clip]{4479F14.ps} \end{figure}$	Figure 12: $\Omega _{\rm m}$ and $\sigma _8$ constraints with the Deep data only. The contours show 0.68, 0.95 and 0.999 confidence regions. Errors include statistical, covariance and residual systematic contributions. The models are pure Cold Dark Matter fit to the data, marginalized over the redshift distribution (see Sect. 7.2 for the details).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,height=5.6cm,clip]{4479F15.ps} \end{figure}$	Figure 13: Same as Fig. 12, combined with the CFHTLS Wide data (Hoekstra et al. 2005). For $\Omega _{\rm m}=0.3$ we have $\sigma _8=0.86\pm 0.05$ at $1 \sigma$ (see Sect. 7.2 for details of the error calculation).
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$\begin{figure} \par\includegraphics[width=7.1cm,height=5.6cm,clip]{4479F16.ps} \end{figure}$	Figure 14: Dark energy constraints from the Deep data only. Hidden parameters are marginalized using a flat prior over $\sigma _8\in [0.7,1.0]$ , $h\in [0.6,0.8]$ and within the $\pm 2\sigma$ boundaries of the redshift parameter $z_{\rm s}$ (see Sect. 7.2).
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