All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{5022fig1.ps}\end{figure}$ Figure 1: R-band image of A697 (North at the top and East to the left) taken with the WFC camera of the INT. Galaxies with successful velocity measurements are labeled as in Table 1. Circles and boxes indicate cluster members and non-member galaxies, respectively. Out of non-member galaxies, bold-face boxes indicate emission-line galaxies. Diamond indicates a QSO at $z\sim 1.50$ . The horizontal spike is due to the presence of a bright star $\sim$ 7 $^\prime$ East of the cluster.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{5022fig2.eps}\end{figure}$ Figure 2: R-band image of the cluster A697 with, superimposed, the contour levels of the Chandra X-ray image ID #4217 (blue, photons in the energy range 0.3-7 keV) and NVSS (Condon et al. 1998) radio image (green, see also Kempner & Sarazin 2001). Red ellipses identify structures detected by Wavdetect. To avoid confusion, only one isodensity contour of the spatial distribution of the (likely) cluster members is shown (magenta, see also Fig. 9). North is at the top and East to the left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5022fig3.eps} \end{figure}$ Figure 3: Redshift galaxy distribution. The solid-line histogram refers to galaxies assigned to the cluster peak according to the adaptive-kernel reconstruction method.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5022fig4.eps} \end{figure}$ Figure 4: Lower panel: rest-frame velocity vs. projected clustercentric distance for the 79 galaxies in the main peak (Fig. 3), where we indicate galaxies rejected by the "shifting gapper'' method (crosses) and emission line galaxies (squares). The remaining 68 fiducial cluster-members (sample-A) are indicated by open circles (out of which blue galaxies are indicated by a small solid circle, see Sect. 3.3). Upper panel: velocity distribution of all 79 galaxies in the main peak (faint solid-line) and 68 member galaxies (dashed line). Velocities of the main and secondary nuclei of the cD galaxy are pointed out (IDs 41 and 42, respectively). In both panels faint vertical lines indicate velocity boundaries of the alternative sample of member galaxies (sample-B, see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5022fig5.eps} \end{figure}$ Figure 5: Differential (solid squares) and integral (small points) profiles of mean velocity ( upper panel) and LOS velocity dispersion ( lower panel). As for the differential profiles, results for six annuli from the cluster center, each of 0.2 h₇₀^-1 Mpc, are shown. As for the integral profiles, the mean and dispersion at a given (projected) radius from the cluster center is estimated by considering all galaxies within that radius - the first point is obtained on the basis of the five galaxies close to the cluster center. In the lower panel, the horizontal line represents the X-ray temperature with the respective 68 per cent errors transformed in $\sigma _{v}$ assuming the density-energy equipartition between gas and galaxies, i.e. $\beta _{\rm spec}=1$ (see text). In both panels differential profiles for red galaxies is also shown (open circles).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5022fig6.eps} \end{figure}$ Figure 6: B-R vs. R diagram for galaxies with available spectroscopy: circles and crosses denote cluster and field members, respectively. Out of field members, squares denote emission line galaxies. The solid line gives the best-fit colour-magnitude relation; the dashed lines are drawn at $\pm$ 0.25 mag from the CMR. According to our working definition in Sect. 3.3 cluster members are divided into blue and red galaxies (below and above the long-dashed line, respectively). In particular, very/not very red galaxies lie above/below the solid line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5022fig7.eps}\end{figure}$ Figure 7: Velocity distribution of radial velocities for the cluster members. Upper and lower panels: stripe density plots where arrow indicate the position of the significant gaps (samples-A and B, respectively). Central panel: velocity histogram with a binning of 100 km s $^{-1} \;$ with the Gaussians corresponding to the most significant KMM partition for the sample-B.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5022fig8.eps}\end{figure}$ Figure 8: Spatial distribution on the sky and relative isodensity contour map of 645 likely cluster members (according to the colour-magnitude relation) with $R\le 21$ , obtained with the adaptive-kernel method (black lines). For comparison we show the contour map of the 749 likely non-cluster members (grey lines). The plot is centered on the cluster center. The circle indicate the 5 $^\prime$ central region.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5022fig9.eps}\end{figure}$ Figure 9: Spatial distribution on the sky and relative isodensity contour map of 149 likely cluster members with $R\le 21$ within 1.3 h₇₀^-1 Mpc $\;$ ( $\sim$ 5 $^\prime$ ) of the cluster center. The plot is centered on the cluster center. Crosses indicate the position of the centers of the substructures found by the wavelet technique in Chandra X-ray data (see Sect. 5).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5022fi10.eps}\end{figure}$ Figure 10: Spatial distribution on the sky and relative isodensity contour map of 54 likely cluster members with $R\le 21$ within 0.6 h₇₀^-1 Mpc $\;$ of the cluster center (gray lines). The contour maps of brilliant and faint galaxies - i.e. galaxies having $R \le 20$ and $20< R\le 21$ - are also shown (black dashed and solid lines, respectively). The plot is centered on the cluster center. Crosses indicate the position of the centers of the substructures found with the wavelet technique in Chandra X-ray data (see Sect. 5).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5022fi11.ps}\end{figure}$ Figure 11: $8.5 \hbox {$^\prime $ }\times 8.5\hbox {$^\prime $ }$ Chandra X-ray image (ID #4217, chip I3 only) of the cluster A697 in the energy band 0.5-2 keV. The circle puts in evidence a faint diffuse emission located $\sim$ 6 $^\prime$ SW from the cluster center (see Sect. 5). North is at the top and East to the left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5022fig3.eps} \end{figure}$	Figure 3: Redshift galaxy distribution. The solid-line histogram refers to galaxies assigned to the cluster peak according to the adaptive-kernel reconstruction method.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5022fig7.eps}\end{figure}$	Figure 7: Velocity distribution of radial velocities for the cluster members. Upper and lower panels: stripe density plots where arrow indicate the position of the significant gaps (samples-A and B, respectively). Central panel: velocity histogram with a binning of 100 km s $^{-1} \;$ with the Gaussians corresponding to the most significant KMM partition for the sample-B.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5022fig9.eps}\end{figure}$	Figure 9: Spatial distribution on the sky and relative isodensity contour map of 149 likely cluster members with $R\le 21$ within 1.3 h₇₀^-1 Mpc $\;$ ( $\sim$ 5 $^\prime$ ) of the cluster center. The plot is centered on the cluster center. Crosses indicate the position of the centers of the substructures found by the wavelet technique in Chandra X-ray data (see Sect. 5).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5022fi11.ps}\end{figure}$	Figure 11: $8.5 \hbox {$^\prime $ }\times 8.5\hbox {$^\prime $ }$ Chandra X-ray image (ID #4217, chip I3 only) of the cluster A697 in the energy band 0.5-2 keV. The circle puts in evidence a faint diffuse emission located $\sim$ 6 $^\prime$ SW from the cluster center (see Sect. 5). North is at the top and East to the left.
Open with DEXTER