Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{0362f01.eps} \end{figure}$ Figure 1: R-band image of A2219 (North at top and East to left). Galaxies with successful velocity measurements are labeled as in Table 1. Circles and boxes indicate cluster member and non-member galaxies, respectively. Labels in bold indicate active galaxies (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0362f02.eps} \end{figure}$ Figure 2: Square root of the redshift galaxy density, as provided by the adaptive-kernel reconstruction method. Units on the y axis are arbitrary.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0362f03.eps} \end{figure}$ Figure 3: Left panel: rest-frame velocities ${v}_{\rm {rf}}$ vs. projected cluster-centric distance r of galaxies in the main peak of Fig. 2. Circles indicate cluster members; crosses indicate the two galaxies rejected by the "shifting gapper'' procedure. Right panel: histogram of rest-frame velocities of selected 113 cluster members. The arrow indicates the cD galaxy velocity.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0362f04.eps} \end{figure}$ Figure 4: Differential (big squares) and integral (small points) mean velocity and line-of-sight velocity dispersion profiles. For the differential profiles, the results for four annuli from the cluster center, each of 0.2 h^-1 Mpc, are shown. 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 error bands at the $68\%$ c.l. are shown. In the lower panel, the horizontal lines represent X-ray temperature with the respective errors transformed in $\sigma _{v}$ (assuming $\beta _{\rm {spec}}=1$ where $\beta _{\rm {spec}}=\sigma _{v}^2/(kT_{\rm X}/\mu m_{\rm p})$ , with $\mu$ the mean molecular weight, $m_{\rm p}$ the proton mass, and $T_{\rm X}$ the X-ray temperature).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0362f05.eps} \end{figure}$ Figure 5: Spatial distribution on the sky of 113 cluster members. Open and solid circles indicate low-and high-velocity galaxies: the larger the symbol, the smaller is the radial velocity. The plot is centered on the cluster center (coincident with the cD galaxy). The solid and faint lines indicate the position angle of the cluster velocity gradient and relative errors, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0362f06.eps} \end{figure}$ Figure 6: Spatial distribution on the sky of the 113 cluster members, each marked by a circle: the larger the circle, 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

$\begin{figure} \par\includegraphics[width=8cm,clip]{0362f07.eps} \end{figure}$ Figure 7: B-R vs. R diagram for galaxies with available spectroscopy: small dots and crosses denote cluster and field members, respectively. Large symbols denotes spectroscopic classified galaxies: circles, triangles, squares, and stars indicate k-, i-, a-, and e-galaxies, respectively. The solid line gives the best-fit CMR; 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 in: blue and red galaxies (below and above the long-dashed line, respectively); very red galaxies lie above the solid line. The left-down region delimited by the dotted lines defines the locus of Butcher-Oemler galaxies (Sect. 5).
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0362f08.eps} \end{figure}$ Figure 8: Spatial distribution on the sky and relative isodensity contour map of 80 bright cluster (R<19.7 galaxies), obtained with the adaptive-kernel method (cf. Pisani 1993, 1996). The plots are centered on the cluster center. The 1 $\hbox {$^\prime $ }$ circle is centered on the cD galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0362f09a.eps}\par\vspace*{... ...}\par\vspace*{2mm} \includegraphics[width=6.9cm,clip]{0362f09c.eps} \end{figure}$ Figure 9: Same as Fig. 8 but for likely cluster members selected on the basis of the B-I CMR in the photometric sample of Smail et al. (1998). Top panel: the 484 I<22galaxies. Middle and bottom panels: two subsamples corresponding to very red and not very red galaxies (273 and 211 galaxies, respectively).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0362f10.eps} \end{figure}$ Figure 10: R-band image of the cluster A2219 with, superimposed, the contour levels of the Chandra image (blue) and of a low-resolution VLA image (green) by Bacchi et al. (2003). The red ellipses represent the structures detected by Wavdetect. North is at top and East to left.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0362f11.eps} \end{figure}$ Figure 11: Residual map of the elliptical Beta model fit (see text). Solid and dotted contour lines indicate regions with positive and negative residuals, respectively. Ellipses represent the structures detected by Wavdetect.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0362f12.eps} \end{figure}$ Figure 12: Temperature map of A2219. The cluster area is divided in eight numbered sectors ( top panel). Sectors are superimposed to the contour levels of the Chandra image. Ellipses show the four structures detected in the X-ray image. The graph in the bottom panel shows the temperature computed in each sector.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0362f13.eps} \end{figure}$ Figure 13: Softness ratio map of A2219 (see text). Superimposed to the map are the eight sectors (see Fig. 12). Dashed ellipses are the structures detected in the X-ray image and crosses show the positions of the cluster members.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0362f14.eps} \end{figure}$ Figure 14: Spatial distribution on the sky of 113 cluster members. Large symbols denotes spectroscopic classified galaxies: circles, triangles, squares, and stars indicate k-, i-, a-, and e-galaxies, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0362f15.eps} \end{figure}$ Figure 15: Optical-mid IR spectral energy distribution of galaxy No. 42. The best-fit GRASIL model is also shown (solid tree).
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0362f01.eps} \end{figure}$	Figure 1: R-band image of A2219 (North at top and East to left). Galaxies with successful velocity measurements are labeled as in Table 1. Circles and boxes indicate cluster member and non-member galaxies, respectively. Labels in bold indicate active galaxies (see text).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0362f02.eps} \end{figure}$	Figure 2: Square root of the redshift galaxy density, as provided by the adaptive-kernel reconstruction method. Units on the y axis are arbitrary.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0362f03.eps} \end{figure}$	Figure 3: Left panel: rest-frame velocities ${v}_{\rm {rf}}$ vs. projected cluster-centric distance r of galaxies in the main peak of Fig. 2. Circles indicate cluster members; crosses indicate the two galaxies rejected by the "shifting gapper'' procedure. Right panel: histogram of rest-frame velocities of selected 113 cluster members. The arrow indicates the cD galaxy velocity.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0362f05.eps} \end{figure}$	Figure 5: Spatial distribution on the sky of 113 cluster members. Open and solid circles indicate low-and high-velocity galaxies: the larger the symbol, the smaller is the radial velocity. The plot is centered on the cluster center (coincident with the cD galaxy). The solid and faint lines indicate the position angle of the cluster velocity gradient and relative errors, respectively.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0362f06.eps} \end{figure}$	Figure 6: Spatial distribution on the sky of the 113 cluster members, each marked by a circle: the larger the circle, 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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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0362f08.eps} \end{figure}$	Figure 8: Spatial distribution on the sky and relative isodensity contour map of 80 bright cluster (R<19.7 galaxies), obtained with the adaptive-kernel method (cf. Pisani 1993, 1996). The plots are centered on the cluster center. The 1 $\hbox {$^\prime $ }$ circle is centered on the cD galaxy.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0362f09a.eps}\par\vspace{... ...}\par\vspace{2mm} \includegraphics[width=6.9cm,clip]{0362f09c.eps} \end{figure}$	Figure 9: Same as Fig. 8 but for likely cluster members selected on the basis of the B-I CMR in the photometric sample of Smail et al. (1998). Top panel: the 484 I<22galaxies. Middle and bottom panels: two subsamples corresponding to very red and not very red galaxies (273 and 211 galaxies, respectively).
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$\begin{figure} \par\includegraphics[width=16cm,clip]{0362f10.eps} \end{figure}$	Figure 10: R-band image of the cluster A2219 with, superimposed, the contour levels of the Chandra image (blue) and of a low-resolution VLA image (green) by Bacchi et al. (2003). The red ellipses represent the structures detected by Wavdetect. North is at top and East to left.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0362f11.eps} \end{figure}$	Figure 11: Residual map of the elliptical Beta model fit (see text). Solid and dotted contour lines indicate regions with positive and negative residuals, respectively. Ellipses represent the structures detected by Wavdetect.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0362f12.eps} \end{figure}$	Figure 12: Temperature map of A2219. The cluster area is divided in eight numbered sectors ( top panel). Sectors are superimposed to the contour levels of the Chandra image. Ellipses show the four structures detected in the X-ray image. The graph in the bottom panel shows the temperature computed in each sector.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0362f13.eps} \end{figure}$	Figure 13: Softness ratio map of A2219 (see text). Superimposed to the map are the eight sectors (see Fig. 12). Dashed ellipses are the structures detected in the X-ray image and crosses show the positions of the cluster members.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0362f14.eps} \end{figure}$	Figure 14: Spatial distribution on the sky of 113 cluster members. Large symbols denotes spectroscopic classified galaxies: circles, triangles, squares, and stars indicate k-, i-, a-, and e-galaxies, respectively.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0362f15.eps} \end{figure}$	Figure 15: Optical-mid IR spectral energy distribution of galaxy No. 42. The best-fit GRASIL model is also shown (solid tree).
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