All Figures

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3168f01.ps} \end{figure}$ Figure 1: Comparison of effective radii obtained for the CDFS field on the HST+ACS image and on the VLT+FORS1 one.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3168f04.ps} \end{figure}$ Figure 4: The correlation of the Sérsic index with the luminosity. Triangles are the Coma cluster data of Gutiérrez et al. (2004), circles and squares are our $z \sim 1$ galaxies in the CDFS and 0055-269 fields respectively and empty symbols are for galaxies with z < 0.88, while filled ones are for our redshift range 0.88< z <1.3.
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{3168f05.ps} \end{figure}$ Figure 5: The fundamental plane as obtained by Jørgensen et al. (1995a,b) for the Coma galaxies (triangles). Symbols are as in Fig. 4. The dashed line represents the best-fit plane to the Coma galaxies as seen edge-on. The small dots represent the GalICS model galaxies (see Sect. 5.2).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3168f06.ps} \end{figure}$ Figure 6: 1-sigma (solid) and 90% (dashed) confidence regions of the joint distribution of the FP parameters $\alpha$ and $\beta$ , for our data-set of $z \sim 1$ galaxies, and for the Coma cluster sample of JFK96.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f07.ps} \end{figure}$ Figure 7: Mass to light ratio vs. mass for our galaxies at $z \sim 1$ and for galaxies in Coma. Symbols are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3168f08.ps} \end{figure}$ Figure 8: Evolution of the mass to light ratio for our galaxies. Symbols are as in Fig. 4 and the continuous line is the linear fit obtained by van Dokkum & Stanford (2003) for the evolution of the mass to light ratio of cluster massive spheroids up to z=1.27. The other lines are obtained with simple stellar population models using the Chabrier (2003) IMF with a formation redshift of 5.0, 3.0, 1.5 and 1.0 ( top to bottom).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f09.ps} \end{figure}$ Figure 9: The Faber-Jackson relation in the rest-frame B-band for our galaxies at $z \sim 1$ and for galaxies in Coma. Symbols are as in Fig. 4, small dots as in Fig. 5, the dashed line is the relation obtained at z=0 by Forbes & Ponman (1999).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f10.ps} \end{figure}$ Figure 10: The Kormendy relation in the rest-frame B-band for our galaxies at $z \sim 1$ and for galaxies in Coma. Symbols are as in Fig. 4 and small dots as in Fig. 5. The dashed line corresponds to M_B=-20.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f11.ps} \end{figure}$ Figure 11: The Faber-Jackson relation in the rest-frame K-band for our galaxies at $z \sim 1$ . Symbols are as in Fig. 4, the dashed line is the local relation obtained for Coma cluster galaxies by Pahre et al. (1998).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f12.ps} \end{figure}$ Figure 12: The comparison of dynamical and stellar masses for our sample at $z \sim 1$ . Symbols are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f13.ps} \end{figure}$ Figure 13: The differential evolution of the ${\cal M}/L_B$ ratio for each individual galaxy of our sample with respect to that of old cluster massive galaxies at the same redshift (see text). Symbols are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3168f14.ps} \end{figure}$ Figure 14: The dependence of the differential evolution in ${\cal M}/L_B$ on the rest-frame equivalent width of the [OII]3727 emission line for our spheroidal galaxies at $z \sim 1$ . Symbols are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3168f15.ps} \end{figure}$ Figure 15: The dependence of the differential evolution in ${\cal M}/L_B$ on the rest-frame U-B color. Symbols are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{3168f02.ps} \end{figure}$ Figure 2: The extracted spectra of all the galaxies for which we could obtain the velocity dispersion.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{3168f03.ps} \end{figure}$ Figure 3: Images of our galaxies from the CDFS field (3 panels on the left: HST+ACS+F435W, HST+ACS+F606W, HST+ACS+F850LP, from left to right) and from the 0055-269 field ( right most panel, VLT+FORS1+Gunn z). Each box is $3\times 3$ arcsec. The numbers in the boxes are the last 3 digits of the object's name (see Table 1).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3168f01.ps} \end{figure}$	Figure 1: Comparison of effective radii obtained for the CDFS field on the HST+ACS image and on the VLT+FORS1 one.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3168f04.ps} \end{figure}$	Figure 4: The correlation of the Sérsic index with the luminosity. Triangles are the Coma cluster data of Gutiérrez et al. (2004), circles and squares are our $z \sim 1$ galaxies in the CDFS and 0055-269 fields respectively and empty symbols are for galaxies with z < 0.88, while filled ones are for our redshift range 0.88< z <1.3.
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$\begin{figure} \par\includegraphics[width=6.1cm,clip]{3168f05.ps} \end{figure}$	Figure 5: The fundamental plane as obtained by Jørgensen et al. (1995a,b) for the Coma galaxies (triangles). Symbols are as in Fig. 4. The dashed line represents the best-fit plane to the Coma galaxies as seen edge-on. The small dots represent the GalICS model galaxies (see Sect. 5.2).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3168f06.ps} \end{figure}$	Figure 6: 1-sigma (solid) and 90% (dashed) confidence regions of the joint distribution of the FP parameters $\alpha$ and $\beta$ , for our data-set of $z \sim 1$ galaxies, and for the Coma cluster sample of JFK96.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f07.ps} \end{figure}$	Figure 7: Mass to light ratio vs. mass for our galaxies at $z \sim 1$ and for galaxies in Coma. Symbols are as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f09.ps} \end{figure}$	Figure 9: The Faber-Jackson relation in the rest-frame B-band for our galaxies at $z \sim 1$ and for galaxies in Coma. Symbols are as in Fig. 4, small dots as in Fig. 5, the dashed line is the relation obtained at z=0 by Forbes & Ponman (1999).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f10.ps} \end{figure}$	Figure 10: The Kormendy relation in the rest-frame B-band for our galaxies at $z \sim 1$ and for galaxies in Coma. Symbols are as in Fig. 4 and small dots as in Fig. 5. The dashed line corresponds to M_B=-20.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f11.ps} \end{figure}$	Figure 11: The Faber-Jackson relation in the rest-frame K-band for our galaxies at $z \sim 1$ . Symbols are as in Fig. 4, the dashed line is the local relation obtained for Coma cluster galaxies by Pahre et al. (1998).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f12.ps} \end{figure}$	Figure 12: The comparison of dynamical and stellar masses for our sample at $z \sim 1$ . Symbols are as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3168f13.ps} \end{figure}$	Figure 13: The differential evolution of the ${\cal M}/L_B$ ratio for each individual galaxy of our sample with respect to that of old cluster massive galaxies at the same redshift (see text). Symbols are as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3168f14.ps} \end{figure}$	Figure 14: The dependence of the differential evolution in ${\cal M}/L_B$ on the rest-frame equivalent width of the [OII]3727 emission line for our spheroidal galaxies at $z \sim 1$ . Symbols are as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3168f15.ps} \end{figure}$	Figure 15: The dependence of the differential evolution in ${\cal M}/L_B$ on the rest-frame U-B color. Symbols are as in Fig. 4.
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$\begin{figure} \par\includegraphics[width=14.5cm,clip]{3168f02.ps} \end{figure}$	Figure 2: The extracted spectra of all the galaxies for which we could obtain the velocity dispersion.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{3168f03.ps} \end{figure}$	Figure 3: Images of our galaxies from the CDFS field (3 panels on the left: HST+ACS+F435W, HST+ACS+F606W, HST+ACS+F850LP, from left to right) and from the 0055-269 field ( right most panel, VLT+FORS1+Gunn z). Each box is $3\times 3$ arcsec. The numbers in the boxes are the last 3 digits of the object's name (see Table 1).
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