All Figures

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{3384fig1CMJN.eps} % \end{figure}$ Figure 1: Color image of the Abell 2667 cluster core imaged with HST in the F450W, F606W, and F814W filters. The thin yellow square represents the position of the IFU field-of-view. Note the strongly magnified gravitational arc and the extended blue region just NE of the central galaxy. The white lines correspond to iso-mass contours from the lens model; the red line is the critical line at the redshift of the giant arc. High-z objects discussed in the text are also marked. North is at the top, East to the left. The field of view is centered on $\alpha _{J2000}$ = 23:51:39.4, $\delta _{J2000}$ = -26:05:03. At a redshift of z=0.233, the angular scale is 3.722 kpc/arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm]{3384fig2.eps}\end{figure}$ Figure 2: Distribution of the rms residuals in the wavelength calibration for all the useful fibers in the first pointing. The median value is 0.716 Å, i.e. 0.15 pixel. 95% of the fiber has rms lower than 1.0 Å.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.5cm,clip]{3384fig3.eps}\end{figure}$ Figure 3: Distribution of the average fiber flux values between 4000 and 6200 Å in the four quadrants of the fully reduced data-cube, showing the uniformity of the background in the different quadrants. In all quadrants, distributions are centered around zero, with standard deviation $0.7 {-} 1.1 \times 10^{18} ~ {\rm erg ~ cm}^{-2} ~\rm \AA^{-1} ~ s^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3384fig4.eps}\end{figure}$ Figure 4: VIMOS-IFU bi-dimensional color image of the central region of the cluster Abell 2667. The blue, green, and red color channels were built by averaging the flux in the spectral ranges: 4500-4700 Å, 4900-5400 Å, and 5700-6200 Å, respectively. The orientation is the same as in Fig. 1. The blue region just NE of the cD galaxy corresponds to an extended emission-line region at the same redshift as the cD. The 21 galaxies with secure redshift measurement (excluding the lensed sources A and Ra) are identified in the plot.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm]{3384fig5.eps}\end{figure}$ Figure 5: Completeness of the redshift survey as a function of V-band magnitude (measured in a 2'' aperture). In the upper panel, we plot the number of objects detected on the HST $\chi ^2$ -image within the VIMOS-IFU f.o.v. (black line) and the number of those object with measured redshift (red line). In the lower panel, the efficiency of the spectroscopic survey is given. The redshift of a bright object at $V \simeq 21.5$ (ID = 15) was not measured since it is located on a set of dead fibers.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3384fig6.eps}\end{figure}$ Figure 6: Color-magnitude relation of the galaxies in VIMOS-IFU f.o.v and detected in the HST $\chi ^2$ -image, using the two WFPC2 pass-bands covering the LR-B spectral range ( F450W and F606W). Filled symbols correspond to objects with measured redshift, empty symbols to objects with no redshift measurement. The cD galaxy (ID = 1) is the brightest object in the diagram. However, becauseof the blue excess associated with the extended emission line region, it lies outside the well-defined cluster red sequence.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm]{3384fig7.eps}\end{figure}$ Figure 7: Redshift distribution of galaxies in the vicinity of the cluster. The bulk of the galaxies are bounded to the cluster centered at z=0.233 with a velocity dispersion of 960 km s^-1 (overlayed Gaussian profile). The arrow marks the position of the central galaxy. Bin size is $\Delta z = 0.002$ , and velocities relative to the cluster rest frame are shown on the top axis (in km s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3384fig8.eps}\end{figure}$ Figure 8: Four representative spectra of cluster members from the VIMOS-IFU survey of A2667 core, in order of decreasing luminosity. Only a few of the detected lines are indicated. Spectra have been smoothed at the instrumental resolution. Shaded region are strongly affected by sky lines residuals.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3384fig9.eps}\end{figure}$ Figure 9: VIMOS-IFU spectra of the three giant-arc components. Individual spectra are obtained by averaging the flux of the fibers at the image positions. Spectra have been box-car smoothed. Vertical lines show the position of the identified UV absorption features. The redshift of the source is $z_{\rm arc} = 1.0334$ . Shaded regions mark the spectral ranges dominated by sky-line residuals.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.9cm,clip]{3384fi10.ps}\end{figure}$ Figure 10: VIMOS-IFU spectrum of the red object Ra (black line, smoothed at the instrumental resolution), together with a redshifted spectrum of a local early-type galaxy (red line). The spectroscopic redshift is based mainly on the identification of the 4000 Å break.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3384fi11.ps}\end{figure}$ Figure A.1: The flux limits for the detection of emission lines sources in two different quadrants (Q1, upper curve, and Q2, lower curve) as a function of the wavelength. The curves for the other two quadrants fall between the two plotted here. See text for details.

In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{3384fi12.eps}\end{figure}$ Figure A.2: 2D map of the sky background rms, considering a window that is $\delta \lambda = 40$ Å wide at $\lambda = 5000$ Å. A logarithmic scale from 10^-19 to 10^-18 erg cm^-2 s^-1 Å^-1 is used, with darker grey corresponding to lower sky levels.

In the text

$\begin{figure} \par\includegraphics[width=7.8cm]{3384fig2.eps}\end{figure}$	Figure 2: Distribution of the rms residuals in the wavelength calibration for all the useful fibers in the first pointing. The median value is 0.716 Å, i.e. 0.15 pixel. 95% of the fiber has rms lower than 1.0 Å.
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$\begin{figure} \par\includegraphics[angle=270,width=7.5cm,clip]{3384fig3.eps}\end{figure}$	Figure 3: Distribution of the average fiber flux values between 4000 and 6200 Å in the four quadrants of the fully reduced data-cube, showing the uniformity of the background in the different quadrants. In all quadrants, distributions are centered around zero, with standard deviation $0.7 {-} 1.1 \times 10^{18} ~ {\rm erg ~ cm}^{-2} ~\rm \AA^{-1} ~ s^{-1}$ .
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$\begin{figure} \par\includegraphics[width=7.6cm]{3384fig7.eps}\end{figure}$	Figure 7: Redshift distribution of galaxies in the vicinity of the cluster. The bulk of the galaxies are bounded to the cluster centered at z=0.233 with a velocity dispersion of 960 km s^-1 (overlayed Gaussian profile). The arrow marks the position of the central galaxy. Bin size is $\Delta z = 0.002$ , and velocities relative to the cluster rest frame are shown on the top axis (in km s^-1).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3384fig8.eps}\end{figure}$	Figure 8: Four representative spectra of cluster members from the VIMOS-IFU survey of A2667 core, in order of decreasing luminosity. Only a few of the detected lines are indicated. Spectra have been smoothed at the instrumental resolution. Shaded region are strongly affected by sky lines residuals.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3384fig9.eps}\end{figure}$	Figure 9: VIMOS-IFU spectra of the three giant-arc components. Individual spectra are obtained by averaging the flux of the fibers at the image positions. Spectra have been box-car smoothed. Vertical lines show the position of the identified UV absorption features. The redshift of the source is $z_{\rm arc} = 1.0334$ . Shaded regions mark the spectral ranges dominated by sky-line residuals.
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$\begin{figure} \par\includegraphics[angle=270,width=7.9cm,clip]{3384fi10.ps}\end{figure}$	Figure 10: VIMOS-IFU spectrum of the red object Ra (black line, smoothed at the instrumental resolution), together with a redshifted spectrum of a local early-type galaxy (red line). The spectroscopic redshift is based mainly on the identification of the 4000 Å break.
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