Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9731fig1.ps}\end{figure}$ Figure 1: r-band image of the Abell 2163 field. The zoomed image shows the bright elliptical galaxy identified as the centre of the cluster from X-ray maps: also visible are the faint gravitational arcs.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.1cm,clip]{9731fig2.ps} \end{figure}$ Figure 2: Selection of galaxies used for the lensing analysis (area with oblique lines) and of the stars used for the PSF correction (area with horizontal lines) in the CFHT-Megacam r-band image; $r_{\rm h}$ is the half-light radius.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.7cm,clip]{9731fig3.ps} \end{figure}$ Figure 3: PSF correction: the first three panels show the spatial pattern of the observed, fitted and residual ellipticities of stars: a scaling factor was applied for display purposes; X and Y are the pixel coordinates in the image. The last panel shows the observed versus corrected ellipticities.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{9731fig4.ps}\vspace*{5mm} \includegraphics[width=6cm,clip]{9731fig5.ps} \end{figure}$ Figure 4: S-maps obtained by aperture densitometry and convolution with up: a Gaussian filter function (size: 5 arcmin); down: the filter function proposed by Schirmer (2004). The contour levels are plotted at S=(3,4,5,6,7), where S is defined in Sect. 3.1.1. The small box indicates the position of the elliptical galaxy with arcs. The dashed contours show for comparison the density distribution of cluster galaxies (see also Maurogordato et al. 2008).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.2cm,clip]{9731fig6.ps} \end{figure}$ Figure 5: Mass profile obtained by aperture densitometry.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{9731fig7.eps} \end{figure}$ Figure 6: The tangential component of the shear (dark points) is displayed as a function of the distance from the assumed centre of the cluster. The lines show the result of the best-fit to the unbinned data using: a NFW profile with $c_{\rm vir}$ given by Eq. (17) (solid line), and a SIS profile (dashed line). Also shown is the radial component of the shear (diamonds), which is expected to be null in the absence of systematic errors.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9731fig8.ps} \end{figure}$ Figure 7: The r-band LF of Abell 2163 compared with other determinations in the literature.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{9731fig9.ps} \end{figure}$ Figure 8: Galaxy counts derived from the control field (empty red circles), compared to literature. The triangles represent the deep counts from the CFH12K-VIRMOS field (McCracken et al. 2003) corrected to the $r_{\rm AB}$ according to Fukugita et al. (1995); the stars mark the counts from the SDSS commissioning data (Yasuda et al. 2001). The error bars of this work take into account only the Poissonian errors ( $\!\sqrt{n}$ /area), whereas for the literature counts the errors are not displayed because they are smaller than the point dimensions.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9731fig10.ps} \end{figure}$ Figure 9: Galaxy counts in the Abell 2163 line of sight (circles) and in the control field (triangles: for display purposes, an offset in r was applied to these points). The lines show the result of the joint fit. The errors bars were computed as described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9731fig1.ps}\end{figure}$	Figure 1: r-band image of the Abell 2163 field. The zoomed image shows the bright elliptical galaxy identified as the centre of the cluster from X-ray maps: also visible are the faint gravitational arcs.
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$\begin{figure} \par\includegraphics[angle=270,width=7.1cm,clip]{9731fig2.ps} \end{figure}$	Figure 2: Selection of galaxies used for the lensing analysis (area with oblique lines) and of the stars used for the PSF correction (area with horizontal lines) in the CFHT-Megacam r-band image; $r_{\rm h}$ is the half-light radius.
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$\begin{figure} \par\includegraphics[angle=270,width=7.7cm,clip]{9731fig3.ps} \end{figure}$	Figure 3: PSF correction: the first three panels show the spatial pattern of the observed, fitted and residual ellipticities of stars: a scaling factor was applied for display purposes; X and Y are the pixel coordinates in the image. The last panel shows the observed versus corrected ellipticities.
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$\begin{figure} \par\includegraphics[angle=270,width=6.2cm,clip]{9731fig6.ps} \end{figure}$	Figure 5: Mass profile obtained by aperture densitometry.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9731fig8.ps} \end{figure}$	Figure 7: The r-band LF of Abell 2163 compared with other determinations in the literature.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9731fig10.ps} \end{figure}$	Figure 9: Galaxy counts in the Abell 2163 line of sight (circles) and in the control field (triangles: for display purposes, an offset in r was applied to these points). The lines show the result of the joint fit. The errors bars were computed as described in the text.
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