Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3232f1.eps} \end{figure}$ Figure 1: The redshift galaxy density, as provided by the adaptive-kernel reconstruction method. Unit on the y-axis is normalized to the density of the highest peak.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3232f2.eps} \end{figure}$ Figure 2: Galaxies in the main peak of Fig. 1. Left panel: rest-frame velocity vs. projected clustercentric distance; the application of the "shifting gapper'' method rejects the galaxies indicated by open squares. Right panel: velocity distribution of all and member galaxies (dotted and solid histograms, respectively).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3232f3.eps} \end{figure}$ Figure 3: Integrated mean velocity and LOS velocity-dispersion profiles ( upper and lower panel, respectively), where $\left <V\right >$ and $\sigma _{\rm V}$ at a given (projected) radius from the cluster center is estimated by considering all galaxies within that radius. The error bands at the $68\%$ c.l. are shown. In the lower panel, the horizontal line represents X-ray temperature with the respective errors transformed into $\sigma _{\rm V}$ imposing $\beta _{\rm spec}=1$ (see Sect. 4).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f4.eps} \end{figure}$ Figure 4: Velocity distribution of radial velocities for the 95 cluster members. Bottom panel: stripe density plot where arrows indicate the position of significant gaps. The first gap lies between 249 757 and 249 997 km s^-1, the second between 251 886 and 252 185 km s^-1, and the third between 252 305 and 252 635 km s^-1. Top panel: velocity histogram with a binning of 500 km s^-1 with the three Gaussians corresponding to KMM1a, KMM1b, and KMM2 in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f5.eps} \end{figure}$ Figure 5: Spatial distribution on the sky of the 95 member galaxies. Open symbols and crosses indicate galaxies assigned to KMM1 and KMM2 groups, respectively (see text). Squares and triangles indicate KMM1a and KMM1b groups, respectively. The plot is centered on the cluster center defined in Sect. 2. Three circular regions, corresponding to regions of extended X-ray emission, are indicated, too (see Fig. 1 by Demarco et al. 2005).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f6.eps} \end{figure}$ Figure 6: Spatial distribution on the sky of the 95 member galaxies: the larger the triangle, the smaller the radial velocity. Open and solid triangles indicate galaxies with velocity lower and higher than the median cluster velocity, respectively. The plot is centered on the cluster center. The big and the small arrows indicate the position angle of the cluster gradient as measured over the whole cluster and in internal regions, respectively. The three circles correspond to the regions of extended X-ray emission.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f7.eps} \end{figure}$ Figure 7: Spatial distribution of cluster members, each marked by a circle: the larger the circle, the larger is the deviation $\delta _i$ of the local parameters from the global cluster parameters, i.e. there is more evidence for substructure (according to the Dressler & Schectman test, see text). The plot is centered on the cluster center.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f8.eps} \end{figure}$ Figure 8: The distribution of $\delta _i$ deviations of the Dressler-Schectman analysis for the 95 member galaxies. The solid line represents the observations, the dashed line the distribution for the galaxies of simulated clusters, normalized to the observed number.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f9.eps} \end{figure}$ Figure 9: Spatial distribution on the sky of the 95 member galaxies. Squares and crosses indicate galaxies assigned to the South-West and East clumps detected by the Dressler-Schectman analysis, respectively (DS-SW and DS-E): thick symbols indicate DS-SW* and DS-E*. Triangles indicate the remaining galaxies of the main system (DS-M).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f10.eps} \end{figure}$ Figure 10: Kinematical profiles of the SW clump obtained assuming the X-ray peak as center. The vertical line indicates the region likely not contaminated from other clumps (see Sect. 3.4). The dashed vertical line indicates the radius of the extended X-ray emission, as defined by Demarco et al. (2005). Top panel: rest-frame velocity vs. projected distance from the clump center: squares and crosses indicate the DS-SW and DS-E as in Fig. 9. Differential (big circles) and integral (small points) mean velocity and LOS velocity-dispersion profiles are shown in middle and bottom panels, respectively. For the differential profiles are plotted: a) the values for eight annuli from the center of the clumps, each of 0.2 Mpc (heavy symbols); the current values of each ten galaxies (faint symbols). For the integral profiles, the mean and dispersion at a given (projected) radius from the clump-center is estimated by considering all galaxies within that radius. The error bands at the $68\%$ c.l. are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f11.eps} \end{figure}$ Figure 11: The same as in Fig. 10, but referring to the E-clump. Note: here the annuli for the differential profiles are 0.45 Mpc each.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f12.eps} \end{figure}$ Figure 12: The same as in Fig. 10, but referring to the central NE-clump.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f13.eps} \end{figure}$ Figure 13: Projected distribution of the 95 member galaxies. Circles, squares, and crosses indicate passive, post-starburst, and emission-lines galaxies, respectively. The three clumps analyzed in Sect. 3.4 are indicated by the three circles and correspond to the regions likely not to be contaminated by galaxies of other clumps, with radii corresponding to vertical lines in Figs. 10-12.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f14.eps} \end{figure}$ Figure 14: The same as in Fig. 10, but considering only passive galaxies. Here the annuli for the differential profiles are 0.3 Mpc each.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f15.eps} \end{figure}$ Figure 15: System mass vs. projection angle for bound and unbound solutions of the two-body model applied to the NE- and SW-clumps (solid and dotted curves, respectively, see text). The thin curve separates the bound and unbound regions according to the Newtonian criterion (above and below the curve, respectively). The horizontal lines give the observational values of the mass system and its 1 $\sigma$ error bands.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3232f1.eps} \end{figure}$	Figure 1: The redshift galaxy density, as provided by the adaptive-kernel reconstruction method. Unit on the y-axis is normalized to the density of the highest peak.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3232f2.eps} \end{figure}$	Figure 2: Galaxies in the main peak of Fig. 1. Left panel: rest-frame velocity vs. projected clustercentric distance; the application of the "shifting gapper'' method rejects the galaxies indicated by open squares. Right panel: velocity distribution of all and member galaxies (dotted and solid histograms, respectively).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f7.eps} \end{figure}$	Figure 7: Spatial distribution of cluster members, each marked by a circle: the larger the circle, the larger is the deviation $\delta _i$ of the local parameters from the global cluster parameters, i.e. there is more evidence for substructure (according to the Dressler & Schectman test, see text). The plot is centered on the cluster center.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3232f8.eps} \end{figure}$	Figure 8: The distribution of $\delta _i$ deviations of the Dressler-Schectman analysis for the 95 member galaxies. The solid line represents the observations, the dashed line the distribution for the galaxies of simulated clusters, normalized to the observed number.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f9.eps} \end{figure}$	Figure 9: Spatial distribution on the sky of the 95 member galaxies. Squares and crosses indicate galaxies assigned to the South-West and East clumps detected by the Dressler-Schectman analysis, respectively (DS-SW and DS-E): thick symbols indicate DS-SW* and DS-E*. Triangles indicate the remaining galaxies of the main system (DS-M).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f11.eps} \end{figure}$	Figure 11: The same as in Fig. 10, but referring to the E-clump. Note: here the annuli for the differential profiles are 0.45 Mpc each.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f12.eps} \end{figure}$	Figure 12: The same as in Fig. 10, but referring to the central NE-clump.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f13.eps} \end{figure}$	Figure 13: Projected distribution of the 95 member galaxies. Circles, squares, and crosses indicate passive, post-starburst, and emission-lines galaxies, respectively. The three clumps analyzed in Sect. 3.4 are indicated by the three circles and correspond to the regions likely not to be contaminated by galaxies of other clumps, with radii corresponding to vertical lines in Figs. 10-12.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3232f14.eps} \end{figure}$	Figure 14: The same as in Fig. 10, but considering only passive galaxies. Here the annuli for the differential profiles are 0.3 Mpc each.
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