Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig1.eps} \end{figure}$ Figure 1: The E (black area) and B-modes (light/green area) aperture mass statistics computed from the residual shapes of the stars after correcting using on of the six PSF models discussed in the text. The areas indicate the $1\sigma$ regions around the mean.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig2.eps} \end{figure}$ Figure 2: Top panel: E (filled points) and B(open points) mode aperture mass measurements as measured from the previous analysis. It uses model-1 (see Table 1) to describe the PSF anisotropy with the wrong centroid estimate and no sigma clipping on the shape parameters of the selected stars. Bottom panel: results using model 6 and the improved catalogues. Because of a different object selection in the new version, we ensured that we only used objects that are in common to produce this figure. The new catalogue contains more galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig3a.eps}\hspace*{4mm} \includegraphics[width=7.75cm,clip]{1513fig3b.eps} \end{figure}$ Figure 3: Panel a) E and B mode shear correlation function (filled and open points, respectively) as measured from the VIRMOS-Descart data; panel b) E and B mode measurements for the aperture mass statistic; panel c) as before but now for the top-hat variance. For all three statistics we observe the signal is consistent with no B-mode on large scales, and a hint of minor contamination on small scales.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig4.eps} \end{figure}$ Figure 4: The shades (red) area corresponds to the $1\sigma$ area around the mean shear correlation function $\langle\gamma(r)\gamma(\theta+r)\rangle$ measured from the VIRMOS-Descart data. The points with error bars show the residual systematics correlation function $\xi _{\rm SYS}$ as defined in the text. The indicated error bars are those of the shear correlation function, and are displayed to show the level of systematics with respect to the 1- $\sigma$ statistical error.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig5.ps} \end{figure}$ Figure 5: Constraints on $\sigma _8$ and $\Omega _{\rm M}$ for a flat CDM Universe, adopting the non-linear prediction given by Smith et al. (2003). The contours correspond to the 0.68, 0.95and 0.999 confidence levels. The solid dark vertical line indicates $\Omega =0.3$ and the horizontal line indicates the maximum of the likelihood for $\sigma _8$ at $\Omega =0.3$ . The models are marginalised over $\Gamma \in [0.1,0.3]$ and $z_{\rm s}\in [0.4,0.48]$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig6.eps} \end{figure}$ Figure 6: $\sigma _8$ probability distribution functions for $\Omega _{\rm M}=0.3$ . Dashed curve is for Peacock & Dodds (1996) (high normalisation), and the solid curve for Smith et al. (2003) (low normalisation). The superimposed dotted lines indicate a Gaussian fit to the likelihood function.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig7.ps} \end{figure}$ Figure 7: VIRMOS-Descart data constraints in the $\Omega _\Lambda -\Omega _{\rm M}$ plane. The models are normalised to the WMAP results ( $\sigma _8=0.9\pm 0.1$ ), and we assumed the priors $\Gamma =[0.1,0.5]$ and $z_{\rm s}=[0.4,0.48]$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig1.eps} \end{figure}$	Figure 1: The E (black area) and B-modes (light/green area) aperture mass statistics computed from the residual shapes of the stars after correcting using on of the six PSF models discussed in the text. The areas indicate the $1\sigma$ regions around the mean.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig6.eps} \end{figure}$	Figure 6: $\sigma _8$ probability distribution functions for $\Omega _{\rm M}=0.3$ . Dashed curve is for Peacock & Dodds (1996) (high normalisation), and the solid curve for Smith et al. (2003) (low normalisation). The superimposed dotted lines indicate a Gaussian fit to the likelihood function.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1513fig7.ps} \end{figure}$	Figure 7: VIRMOS-Descart data constraints in the $\Omega _\Lambda -\Omega _{\rm M}$ plane. The models are normalised to the WMAP results ( $\sigma _8=0.9\pm 0.1$ ), and we assumed the priors $\Gamma =[0.1,0.5]$ and $z_{\rm s}=[0.4,0.48]$ .
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