All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H4523F01.eps} \end{figure}$ Figure 1: Sky distribution of the GaBoDS fields. The size of the symbols depicts the covered sky area. All fields are at high galactic latitude.
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In the text

$\begin{figure} \includegraphics[width=8.6cm,clip]{H4523F02.eps} \end{figure}$ Figure 2: Exposure times in GaBoDS. The peak at 56 ksec represents the Chandra Deep Field South (CDF-S).
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{H4523F03.eps} \end{figure}$ Figure 3: PSF anisotropies for an intrafocal (upper left), focal (upper right) and extrafocal (lower left) exposure. The chosen scale for the stick length is the same for those three plots in order to show the increase in the anisotropies with respect to the focused exposure. The mean stellar ellipticities are 6.6%, 0.9% and 5.9%, respectively. The lower right panel depicts typical PSF anisotropies of a stacked WFI@2.2 R-band image ( $\sim$ 50 exposures with $\sim$ 500 s exposure time each). Note that the largest PSF anisotropy in the stacked image is as small as 0.8%. Compared to the other three PSF plots a different scale for the stick length was used in order to clearly show the anisotropies.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{H4523F04.eps} \end{figure}$ Figure 4: Difference in object position between a single-shift approach and a full two-dimensional second order astrometric solution for the WFI@2.2. In other words, shown are the higher order terms needed for matching the CCDs to the sky. The patterns belonging to the left two chips are due to a rotation with respect to the mosaic. The maximum position difference in the plot is about six pixels, still a fairly small value compared to other telescope designs. It becomes clear that a single, global distortion polynomial for all CCDs does not work. Instead, every CCD has to be treated individually.
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In the text

$\begin{figure} \includegraphics[width=8.8cm,clip]{H4523F05.eps} \end{figure}$ Figure 5: Coadded weight image of a small WFI@2.2 data set consisting of five exposures. One clearly identifies regions with less effective exposure time due to gaps between CCDs and different pixel sensitivities. The size of the dither pattern also becomes obvious. Brighter regions correspond to pixels with higher weight. The variations from chip to chip are due to differences in the gain and the flatfield.
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In the text

$\begin{figure} \par\includegraphics[width=13.4cm,clip]{H4523F06.eps} \end{figure}$ Figure 6: PSF anisotropies in the NGC 300 R-band image. Upper left: before correction, upper right: after correction. Lower left: Anisotropies as measured in the image, lower right: a two-dimensional polynomial fit to the PSF anisotropies.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4523F07.eps} \end{figure}$ Figure 7: Photometric redshift distribution for the Chandra Deep Field South, determined from UBVRI WFI@2.2 photometry. The redshifts were estimated with hyperz (solid line) (Bolzonella et al. 2000). Only objects that had a good redshift fit of $P(\chi ^2)>0.9$ went into the distribution shown. The dash-dotted line shows an independent measurement of the photometric redshifts from E. Hatziminaoglou (ESO) for the same data set (private communication). The peak at z=2.8 is due to a degeneracy between low and high redshift galaxies and appeared since no prior for the luminosity of galaxies was used. These excess objects are randomly drawn from the low-z regime. Thus the main peak of this distribution was lowered, but not shifted in redshift. Equation (12) was fitted to both distributions, yielding consistent values $z_{0}=0.373\;(0.377)$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{H4523F08.eps} \end{figure}$ Figure 8: The expected S/N ratios for various massive dark matter haloes, as detected with $M_{\rm ap}$ in the NGC 300 WFI@2.2 field. The effect of a background galaxy population with higher redshift is shown, too.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{H4523F09.eps} \end{figure}$ Figure 9: The $M_{\rm ap}$ statistics for various filter scales: 3$.^$2 (upper left), 4$.^$0 (upper right), 5$.^$6 (lower left) and 8$.^$0 (lower right). Shown are $M_{\rm ap}$ probability contours drawn from 5000 randomisations each. The contours depict the 2.0, 2.5, 3.0, 3.5 $\sigma$ levels. The cluster CL0056.03 can be found left of the brightest star, and CL0056.02 sits in the lower left corner. See also Figs. 13 and 14 for comparison. The large elliptical contour arises from the fact that $M_{\rm ap}$ can not determine any value for the pixels inside the contour, since for those no galaxies lie inside the filter. Thus, the distance from this ellipse to the outer edge of the mask depicts the radius of the $M_{\rm ap}$ filter function.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{H4523F11.eps} \end{figure}$ Figure 10: A 100 ksec XMM observation of the NGC 300 field. Shown are X-ray (0.3-6.0 keV) contours and the XMM field of view, superimposed on the optical WFI data. The circles indicate the positions of CL0056.03 (upper left), clump "A'' (left), clump "C'' (upper right) and the $M_{\rm ap}$ peak that lies behind NGC 300 (lower right).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{H4523F10.eps} \end{figure}$ Figure 11: The (V-R,R)-colour-magnitude diagram for all galaxies around NGC 300. The selected cluster sequence for CL0056.03 and CL0056.02 is marked by the large box. Besides, we checked all galaxies with R>23 for spatial clustering. Only the redder objects in the upper aperture show significant clustering properties. Find more details in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{H4523F12.eps} \end{figure}$ Figure 12: Shown are predictions for the WFI@2.2 V-R colours of elliptical galaxies as a function of redshift (Bruzual & Charlot 1993; Bolzonella et al. 2000). Based on the track that includes evolutionary effects we estimate the redshifts for the shear-selected red clumps.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{H4523F13.eps} \end{figure}$ Figure 13: Galaxies inside the lower red cluster sequence of Fig. 11 are shown as big dots. The small dots indicate galaxies brighter than R=21 which do not fall inside the red sequence window. The overlaid contours are isodensity contours for the red sequence members, smoothed at a 3$.^$6 scale, and starting with the $1\sigma$ -overdensity contour in steps of $1\sigma$ . CL0056.03 and CL0056.02 are detected at the $8\sigma$ and $5\sigma$ level respectively. CL0056.03 appears strongly elongated, with an intersecting 12 $\;\!\!^{\prime}$ long filament extending north-south at its eastern side. Part of the filament could belong to Abell S0102 at $(\alpha ,\delta )=(13.91,-37.41)$ , a poor cluster at z=0.05. Galaxies with measured spectra are highlighted with small squares around them.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{H4523F14.eps} \end{figure}$ Figure 14: Shown is the distribution of galaxies inside the upper red cluster sequence of Fig. 11 (big dots). The small dots indicate galaxies brighter than R=22.5 which do not fall inside the red sequence window. Clump "A'' is a very tight concentration of nine galaxies with R<22.3 within 25 $\;\!\!^{\prime\prime}$ . There are five more galaxies spread along a 1 $\;\!\!^{\prime}$ filament to the east and to the west. Clump "B'' is a much looser, 4 $\;\!\!^{\prime}$ long filament consisting of 13 galaxies without a central concentration. In the centre of the filament one finds a R=19.4 bright elliptical, about 1 magnitude brighter than the second brightest member of this concentration. Clump "C'' consists of 6 galaxies within 80 $\;\!\!^{\prime\prime}$ , the brightest one with a R-magnitude of 20.9. Finally, clump "D'' is a very loose grouping of fainter red galaxies that looks like a chance alignment rather than a cluster. Note that the resolution of this plot is not high enough to reveal all candidate galaxies. The smoothing length for the density contours was 1$.^$5 arcmin. Clumps "A'' and "C'' lie within $\sim$ $50\hbox{$\;\!\!^{\prime\prime}$ }$ of weak lensing peaks.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{H4523F15.eps} \end{figure}$ Figure 15: Colour-magnitude diagrams for galaxies inside the cluster sequence window. Galaxies with spectroscopically determined redshifts are marked with squares, the cD galaxies are indicated with a double square (they also have measured redshifts). The galaxy with R=19 and V-R=0.73, marked with a diamond symbol, has z=0.27, higher than the cluster redshift. Furthermore, galaxies were split into three distance bins as seen from the geometrical cluster centre. The outer radii (635 kpc respectively 385 kpc) of the second annuli were chosen in a way that galaxies in the third, outer annulus do not show an apparent concentration with respect to the red cluster sequence any more. Isodensity contours in the colour-magnitude space were calculated from all galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{H4523F16.eps} \end{figure}$ Figure 16: Image of CL0056.03. In the left panel the 21 spectroscopically confirmed cluster members are shown, together with the perpendicular bisector of the connection line between the two cD galaxies, which we chose to split the cluster galaxies into two samples. An [OII] emission line galaxy at higher redshift is indicated. The right panel shows a steeper scaled version of the image at left, showing that ${\rm cD_1}$ and ${\rm cD_2}$ are both embedded in large, but well separated haloes.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4523F17.eps} \end{figure}$ Figure 17: The redshifts of the galaxies in CL0056.03 as a function of distance from the geometrical cluster centre. There is a highly significant ( $\sim$ $4\sigma$ ) correlation between galaxy position and redshift, indicating that CL0056.03 actually consists of two possibly merging subclumps. The slope of the linear fit is different from zero on the $4.1\sigma$ level. Note that ${\rm cD_1}$ has a peculiar motion of 780 $\rm{km~s^{-1}}$ with respect to its own clump.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{H4523F01.eps} \end{figure}$	Figure 1: Sky distribution of the GaBoDS fields. The size of the symbols depicts the covered sky area. All fields are at high galactic latitude.
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$\begin{figure} \includegraphics[width=8.6cm,clip]{H4523F02.eps} \end{figure}$	Figure 2: Exposure times in GaBoDS. The peak at 56 ksec represents the Chandra Deep Field South (CDF-S).
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$\begin{figure} \par\includegraphics[width=13.4cm,clip]{H4523F06.eps} \end{figure}$	Figure 6: PSF anisotropies in the NGC 300 R-band image. Upper left: before correction, upper right: after correction. Lower left: Anisotropies as measured in the image, lower right: a two-dimensional polynomial fit to the PSF anisotropies.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{H4523F08.eps} \end{figure}$	Figure 8: The expected S/N ratios for various massive dark matter haloes, as detected with $M_{\rm ap}$ in the NGC 300 WFI@2.2 field. The effect of a background galaxy population with higher redshift is shown, too.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{H4523F11.eps} \end{figure}$	Figure 10: A 100 ksec XMM observation of the NGC 300 field. Shown are X-ray (0.3-6.0 keV) contours and the XMM field of view, superimposed on the optical WFI data. The circles indicate the positions of CL0056.03 (upper left), clump "A'' (left), clump "C'' (upper right) and the $M_{\rm ap}$ peak that lies behind NGC 300 (lower right).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{H4523F10.eps} \end{figure}$	Figure 11: The (V-R,R)-colour-magnitude diagram for all galaxies around NGC 300. The selected cluster sequence for CL0056.03 and CL0056.02 is marked by the large box. Besides, we checked all galaxies with R>23 for spatial clustering. Only the redder objects in the upper aperture show significant clustering properties. Find more details in the text.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{H4523F12.eps} \end{figure}$	Figure 12: Shown are predictions for the WFI@2.2 V-R colours of elliptical galaxies as a function of redshift (Bruzual & Charlot 1993; Bolzonella et al. 2000). Based on the track that includes evolutionary effects we estimate the redshifts for the shear-selected red clumps.
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