All Figures

$\begin{figure} \par\includegraphics[width=11cm,clip]{xy_mag18c.eps} \end{figure}$ Figure 1: Projected density map of the 168 galaxies brighter than $O = 18^{\rm m}$ in the field of Abell 376 together with the positions of the galaxies (pluses). Galaxies with measured redshifts are marked with circles. Back and foreground galaxies (see Sect. 4) are marked with squares. Larger symbols denote brighter galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{Ao3XBW.eps} \end{figure}$ Figure 2: Contours of constant galactic absorption, A_O (labelled), superimposed to the surface density image of galaxies brighter than $O = 18^{\rm m}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{fdl.eps} \end{figure}$ Figure 3: O magnitudes histograms: continuous line: galaxies inside the square region of measured redshifts; the dashed line histogram is for galaxies with measured redshifts (see Fig. 1). Dotted lines: galaxies belonging to the NW condensation.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{D19.5all_x_vel-cont.eps} \end{figure}$ Figure 4: Isopleths of the projected distribution of galaxies with $12~000 ~{\rm km~s^{-1}}< V < 17~000 ~{\rm km~s^{-1}}$ (dashed lines), together with the corresponding ones for APS galaxies brighter than $19.5^{\rm m}$ (continuous lines).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{alp_del376tot.eps} \end{figure}$ Figure 5: Wedge velocity diagram in right ascension (top), and declination (bottom) for the galaxies in the Abell 376 field with measured radial velocities smaller than $V < 30~000~{\rm km~s^{-1}}$ . Abell 376 is situated at $cz \sim 14~500~{\rm km~s^{-1}}$ (thin ellipsis) with a classical elongated shape, surrounded by 403 galaxies with known redshifts within a radius of 300 arcmin from the cluster center.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm]{vit376.eps} \end{figure}$ Figure 6: The radial velocity distribution for the Abell 376 sample of galaxies between 12 000 and $17~000~{\rm km~s^{-1}}$ . The continuous curve shows the Gaussian distribution corresponding to the mean velocity and velocity dispersion quoted in the text (normalized to the sample size and range).
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{A376_dss_red_ASCA_HRI.eps} \end{figure}$ Figure 7: Left: Red DSS image overlayed with ROSAT HRI isocontours. Right: ASCA GIS broad band smoothed image superposed with HRIisocontours.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{A376_HRI_Isopleta.eps} \end{figure}$ Figure 8: ROSAT HRI isocontours (continuous lines) as in Fig. 7 superposed to the isopleths of the projected galaxy distribution (dashed lines, galaxies within $12~000 ~{\rm km~s^{-1}}< V < 17~000 ~{\rm km~s^{-1}}$ ; thin dotted lines, APS galaxies brighter than $19.5^{\rm m}$ ) as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{gis3Abell376mekal.eps} \end{figure}$ Figure 9: ASCA GIS spectrum showing the MEKAL plasma model best fit. The fit shown here have a fixed $N_{\rm H} = 6.76 \times 10^{20}$ cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{class376.eps} \end{figure}$ Figure 10: Projection of the spectra of 54 cluster galaxies on to the plane defined by the first two principal components. The spectral sequence follows the first component and a spectral type, ST, is attributed to each galaxy by its value of this component. Filled circles, open squares, open triangles, and crosses represent E, S0, S0/S, and S galaxies, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{xy_mag18c.eps} \end{figure}$	Figure 1: Projected density map of the 168 galaxies brighter than $O = 18^{\rm m}$ in the field of Abell 376 together with the positions of the galaxies (pluses). Galaxies with measured redshifts are marked with circles. Back and foreground galaxies (see Sect. 4) are marked with squares. Larger symbols denote brighter galaxies.
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$\begin{figure} \par\includegraphics[width=12cm]{Ao3XBW.eps} \end{figure}$	Figure 2: Contours of constant galactic absorption, A_O (labelled), superimposed to the surface density image of galaxies brighter than $O = 18^{\rm m}$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{fdl.eps} \end{figure}$	Figure 3: O magnitudes histograms: continuous line: galaxies inside the square region of measured redshifts; the dashed line histogram is for galaxies with measured redshifts (see Fig. 1). Dotted lines: galaxies belonging to the NW condensation.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{D19.5all_x_vel-cont.eps} \end{figure}$	Figure 4: Isopleths of the projected distribution of galaxies with $12~000 ~{\rm km~s^{-1}}< V < 17~000 ~{\rm km~s^{-1}}$ (dashed lines), together with the corresponding ones for APS galaxies brighter than $19.5^{\rm m}$ (continuous lines).
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$\begin{figure} \par\includegraphics[width=8.7cm]{vit376.eps} \end{figure}$	Figure 6: The radial velocity distribution for the Abell 376 sample of galaxies between 12 000 and $17~000~{\rm km~s^{-1}}$ . The continuous curve shows the Gaussian distribution corresponding to the mean velocity and velocity dispersion quoted in the text (normalized to the sample size and range).
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{A376_dss_red_ASCA_HRI.eps} \end{figure}$	Figure 7: Left: Red DSS image overlayed with ROSAT HRI isocontours. Right: ASCA GIS broad band smoothed image superposed with HRIisocontours.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{A376_HRI_Isopleta.eps} \end{figure}$	Figure 8: ROSAT HRI isocontours (continuous lines) as in Fig. 7 superposed to the isopleths of the projected galaxy distribution (dashed lines, galaxies within $12~000 ~{\rm km~s^{-1}}< V < 17~000 ~{\rm km~s^{-1}}$ ; thin dotted lines, APS galaxies brighter than $19.5^{\rm m}$ ) as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{gis3Abell376mekal.eps} \end{figure}$	Figure 9: ASCA GIS spectrum showing the MEKAL plasma model best fit. The fit shown here have a fixed $N_{\rm H} = 6.76 \times 10^{20}$ cm^-2.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{class376.eps} \end{figure}$	Figure 10: Projection of the spectra of 54 cluster galaxies on to the plane defined by the first two principal components. The spectral sequence follows the first component and a spectral type, ST, is attributed to each galaxy by its value of this component. Filled circles, open squares, open triangles, and crosses represent E, S0, S0/S, and S galaxies, respectively.
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