All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig3.eps} \end{figure}$ Figure 3: Redshift galaxy distribution. The solid line histogram refers to galaxies assigned to the cluster according to the DEDICA reconstruction method.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7407fig4.eps}\end{figure}$ Figure 4: Projected clustercentric distance vs. rest-frame velocity $v_{\rm rf}=(v-\langle v\rangle)/(1+z)$ for the 88 galaxies in the main peak (see Fig. 3) showing galaxies detected as interlopers by our "shifting gapper'' procedure (stars and crosses) when using BCM-A and -B as alternative cluster centres ( top and bottom panels, respectively). We reject the three galaxies with highest velocities (stars) to build our basic sample of 85 galaxies and all galaxies indicated by crosses and stars in the top panel to build our Sample2. The three brightest cluster members each one corresponding to Beers et al. (1983) clumps (BCM-A, -B and -C) and a fourth bright galaxy (BCM-D) are indicated by squares.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig5.eps}\end{figure}$ Figure 5: Top panel: velocity distribution of the 85 fiducial cluster members. Arrows correspond to the bright galaxies BCM-A, -B, -C and -D. Bottom panel: stripe density plot where the arrows indicate the positions of the significant gaps. The gap at the lower velocity has a normalized size =2.41, the other =2.25.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{7407fig6.eps}\end{figure}$ Figure 6: Spatial distribution on the sky of spectroscopically confirmed cluster members and the relative isodensity contour map. The three brightest galaxies BCM-A -B, and -C corresponding to Beers et al. (1983) groups, a fourth bright galaxy (BCM-D) and the X-ray peaks are indicated by large squares, too. The plot is centred on the cluster centre defined as the bi-weight centre (see text).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7407fig7.eps}\end{figure}$ Figure 7: B-R vs. R diagram for galaxies with available spectroscopy is shown by small dots and crosses (cluster and field members, respectively). Large solid dots indicate luminous galaxies BCM-A, -B, -C and -D. The solid line gives the best-fit colour-magnitude relation as determined on member galaxies; the dashed lines are drawn at $\pm$ 0.25 mag from the CMR. Large open symbols indicates classified galaxies: circles ("k''), squares ("k+a''), rombs ("a+k''), triangles ("e(c)''), and stars ("e(a)''/"e(b)'').
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7407fig8.eps}\end{figure}$ Figure 8: Spatial distribution on the sky and relative isodensity contour map of 369 likely cluster members (according to the colour-magnitude relation) with $R\le 21$ , obtained with the DEDICA method. The three brightest galaxies BCM-A -B, and -C are indicated by large circles and the X-ray peaks are indicated by large squares. It is also shown the position of the luminous galaxy BCM-D. The plot is centred on the cluster centre.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7407fig9.eps}\end{figure}$ Figure 9: Spatial distribution on the sky of 85 cluster members. Open and solid circles indicate low and high velocity galaxies, the cross the galaxy with median velocity. The larger the symbol, the smaller is the radial velocity. The solid and faint lines indicate the position angle of the cluster gradient and relative errors, respectively. The faint big squares indicate the 14 galaxies belonging to WGAP1 and WGAP2 (see Sect. 3.2). The plot is centred on the cluster centre.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7407fig10.eps}\end{figure}$ Figure 10: 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 boldface circles indicate those with $\delta _i \ge 2.2$ (see text). The plot is centred on the cluster centre.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig11.eps}\end{figure}$ Figure 11: The distribution of $\delta _i$ deviations of the Dressler-Schectman analysis for the 85 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

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig12.eps}\end{figure}$ Figure 12: Spatial distribution on the sky of the 85 member galaxies. Solid circles, open circles and triangles indicate KMM1, KMM2, and KMM3. The large faint squares indicate the position of the brightest cluster members BCM-A, -B, -C and -D. The plot is centred on the cluster centre.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig13.eps}\end{figure}$ Figure 13: Kinematical profiles of the northern subcluster A115N obtained assuming BCM-A as centre. The vertical line indicates the region likely not contaminated from other galaxy clumps (see text). Top panel: rest-frame velocity vs. projected distance from the subcluster centre (BCM-A): crosses indicate the galaxies belonging to WGAP1 and WGAP2. 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 we plot the values for seven annuli from the centre of the subcluster, each of 0.25 h₇₀^-1 Mpc. For the integral profiles, the mean and dispersion at a given (projected) radius from the subcluster-centre is estimated by considering all galaxies within that radius - the first value computed on the five galaxies closest to the centre. The error bands at the $68\%$ c.l. are also shown. In the bottom panel, the horizontal line represents the range of X-ray temperatures as given in the literature for A115N (see Sect. 1) transformed in $\sigma _{v}$ assuming the density-energy equipartition between gas and galaxies, i.e. $\beta _{\rm spec}=1$ (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig14.eps}\end{figure}$ Figure 14: The same as in Fig. 13, but referring to the southern subcluster A115S centred around BCM-B. The dashed line in the bottom panel gives the integral velocity dispersion profile when rejecting the low velocity galaxies of WGAP1 and WGAP2. In the bottom panel, the horizontal line represents the range of X-ray temperatures as given in the literature for A115S (see Sect. 1) transformed in $\sigma _{v}$ assuming the density-energy equipartition between gas and galaxies, i.e. $\beta _{\rm spec}=1$ (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig15.eps}\end{figure}$ Figure 15: System mass vs. projection angle for bound and unbound solutions of the two-body model applied to A115N and A115S subclusters (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 uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,,angle=180,clip]{7407fig1.ps}\end{figure}$ Figure 1: R-band image of A115 taken with the WFC camera of the INT. Targets with successful velocity measurements are labeled as in Table 1. Circles and boxes indicate cluster members and non member galaxies, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,,angle=180,clip]{7407fig2.ps}\end{figure}$ Figure 2: R-band image of the cluster A115 with, superimposed, the smoothed contour levels of the Chandra X-ray image ID#3233 (photons in the energy range 0.5-5 keV; blue) and the contour levels of the NVSS (Condon et al. 1998) radio image (red). Letters A, B, C and D indicate the three brightest cluster members each one corresponding to Beers et al. (1983) clumps and a fourth bright galaxy (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig3.eps} \end{figure}$	Figure 3: Redshift galaxy distribution. The solid line histogram refers to galaxies assigned to the cluster according to the DEDICA reconstruction method.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig5.eps}\end{figure}$	Figure 5: Top panel: velocity distribution of the 85 fiducial cluster members. Arrows correspond to the bright galaxies BCM-A, -B, -C and -D. Bottom panel: stripe density plot where the arrows indicate the positions of the significant gaps. The gap at the lower velocity has a normalized size =2.41, the other =2.25.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{7407fig6.eps}\end{figure}$	Figure 6: Spatial distribution on the sky of spectroscopically confirmed cluster members and the relative isodensity contour map. The three brightest galaxies BCM-A -B, and -C corresponding to Beers et al. (1983) groups, a fourth bright galaxy (BCM-D) and the X-ray peaks are indicated by large squares, too. The plot is centred on the cluster centre defined as the bi-weight centre (see text).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig11.eps}\end{figure}$	Figure 11: The distribution of $\delta _i$ deviations of the Dressler-Schectman analysis for the 85 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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$\begin{figure} \par\includegraphics[width=8cm,clip]{7407fig12.eps}\end{figure}$	Figure 12: Spatial distribution on the sky of the 85 member galaxies. Solid circles, open circles and triangles indicate KMM1, KMM2, and KMM3. The large faint squares indicate the position of the brightest cluster members BCM-A, -B, -C and -D. The plot is centred on the cluster centre.
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$\begin{figure} \par\includegraphics[width=14.5cm,,angle=180,clip]{7407fig1.ps}\end{figure}$	Figure 1: R-band image of A115 taken with the WFC camera of the INT. Targets with successful velocity measurements are labeled as in Table 1. Circles and boxes indicate cluster members and non member galaxies, respectively.
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