All Figures

$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=11cm]{9926figa.eps}\\ \end{tabular} \end{figure}$ Figure 1: F850LP image, Galfit model image, residual image. For these two objects (J033237.54-274848.9 on the left and J033214.97-275005.5 on the right), the software gives a similar confidence level in the fitting process ( $\chi ^2\simeq 1.4$ ). For J033237.54-274848.9 ( left), the $\chi ^2$ is high due to spiral arms, whereas it is due to the two clumps located southeast of the center for J033214.97-275005.5 ( right).
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In the text

$\begin{figure} \par\includegraphics[height=9cm]{9926figb.eps} \end{figure}$ Figure 2: Decision tree used to morphologically classify the sample. We assign each object a morphological label following step-by-step the arms of the tree. For each morphological class, we also report the number of galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{9926figc.eps} \end{figure}$ Figure 3: B-V-z color images of nine galaxies selected in the CDFS sample with B/T < 0.4. The three galaxies in the first column are classified as spiral disks, those in the second column are Peculiar/Irregulars, and those in the third column are Peculiar/Tadpoles.
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In the text

$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=4.3cm]{9926figd.eps} \end{tabular} \end{figure}$ Figure 4: B-V-z color images of six galaxies representative of the six morphological classes used in this study. From top to bottom and left to right: spiral disks, Peculiar/Irregular, Peculiar/Tadpole, Peculiar/Merger, compact galaxies, and major mergers.
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In the text

$\begin{figure} \par\includegraphics[height=9cm]{9926fige.eps} \end{figure}$ Figure 5: Comparison between the morphological classification and the kinematical classification. Morphological classes are quoted in the bottom of X-coordinate, kinematical classes in Y-coordinate. RD refers to rotating disks, PR to perturbed rotations and CK to complex kinematics.
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In the text

$\begin{figure} \par\includegraphics[height=6cm]{9926figf.eps} \includegraphics[height=6cm]{9926figg.eps} \end{figure}$ Figure 6: top: $\log(A)-\log(C)$ diagram. Bottom: Gini-M20 diagram. Different symbols refer to the morphological classes: spiral disks are represented as blue circles, peculiars as green squares, compact galaxies as black diamonds, and mergers as red triangles.
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In the text

$\begin{figure} \par\includegraphics[height=9cm]{9926figh.eps} \end{figure}$ Figure 7: Comparison between the concentration-assymetry (dotted filled histogram), Gini-M20 (solid histogram) morphological classification, and the kinematical classification. Morphological classes are quoted in the bottom of X-coordinate, kinematical classes in Y-coordinate. RD refers to rotating disks, PR to perturbed rotations and CK to complex kinematics. The line for the CA and Gini/M20 exactly overlap for the RD types.
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In the text

$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=9cm]{9926figi.eps} \end{tabular} \end{figure}$ Figure 8: B₄₃₅-z₈₅₀ ( top) and V₆₀₆-I₈₁₄ ( bottom) observed color as a function of redshift. Three solar metallicity, beginning their evolution at z=5 galaxy models, including an elliptical galaxy (single burst - filled red curve), S0 galaxy ( $\tau =1$ Gyr - orange dotted line), and late type galaxy ( $\tau =7$ Gyr - blue dotted line) are plotted for comparison. A young starburst (assuming $L_v \propto v^{-1}$ - cyan dotted line) is also plotted. Different morphological classes are represented by blue circles for spiral disks, green squares for peculiars, black diamonds for compacts, and red triangles for mergers. The mean error for B₄₃₅-z₈₅₀ plot is 0.03 mag (0.01 mag for V₆₀₆-I₈₁₄ respectively), much smaller than the symbol size.
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In the text

$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=9cm]{9926figj.eps} \end{tabular} \end{figure}$ Figure 9: B₄₃₅-z₈₅₀ ( top) and V₆₀₆-I₈₁₄ ( bottom) observed color of the bulges for the rotating spiral disks sub-sample. The different evolutionary models are the same as in Fig. 8. Error bars are used to show the maximal pixel-by-pixel color range within each bulge.
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In the text

$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=2.8cm]{9926figk.eps}\\ \includegraphics[height=4.5cm]{9926figl.eps} \end{tabular} \end{figure}$ Figure 10: Top: three color images of three rotating spiral disks for which we have identified the star-bursting regions (B-z <1 or V-I<0.4). Middle: color profiles for the CDFS galaxies. Bottom: repartition of the starburst light for a growing elliptical aperture. For each aperture, it represents the integrated UV light coming from pure starburst regions normalized by the UV flux coming from all star-bursting regions.
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In the text

$\begin{figure} \par\includegraphics[height=3.3cm]{9926figm.eps} \end{figure}$ Figure 11: Ratio between stellar mass and SFR $_{\rm tot}$ as a function of galaxy radius. SFR $_{\rm tot}$ is defined as the sum of SFR $_{\rm UV}$ and SFR $_{\rm IR}$ . Only galaxies which have been detected by Spitzer are used in this analysis. The vertical line is at 1/3.2 of $R_{\rm max}$ which roughly corresponds to the disk scale length limit.
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In the text

$\begin{figure} \par\includegraphics[height=20.5cm]{9926fign.eps} \end{figure}$ Figure 12: F850LP/ F814W image, color map. Explanations are given at the end of this figure. Rotating spiral disks are marked with an asterisk near their name.
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In the text

$\begin{figure} \par\includegraphics[height=20.5cm]{9926figo.eps} \end{figure}$ Figure 12: continued.
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In the text

$\begin{figure} \par\includegraphics[height=18cm]{9926figp.eps} \end{figure}$ Figure 12: continued. The size of each image is $20\times 20$ kpc. Galaxies observed with ACS have F850LP images, galaxies in CFRS and HDFS have F814W images. For each target, the name and redshift are labeled at the top-left and top right in the F850LP/ F814W image. Rotating spiral disks are marked with an asterisk near their names. Morphological and kinematic classifications are indicated at the bottom-left and bottom right, respectively. Color maps are B₄₃₅-z₈₅₀ for CDFS objects and V₆₀₆-I₈₁₄ for objects in HDFS and CFRS (except CFRS039003, CFRS030488 with B₄₅₀-I₈₁₄ and CFRS1032 with V₅₅₅-I₈₁₄). All the galaxies are aligned with the GIRAFFE IFU (see Paper I).
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In the text

$\begin{figure} \par\includegraphics[height=9cm]{9926figb.eps} \end{figure}$	Figure 2: Decision tree used to morphologically classify the sample. We assign each object a morphological label following step-by-step the arms of the tree. For each morphological class, we also report the number of galaxies.
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$\begin{figure} \par\includegraphics[width=8cm]{9926figc.eps} \end{figure}$	Figure 3: B-V-z color images of nine galaxies selected in the CDFS sample with B/T < 0.4. The three galaxies in the first column are classified as spiral disks, those in the second column are Peculiar/Irregulars, and those in the third column are Peculiar/Tadpoles.
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$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=4.3cm]{9926figd.eps} \end{tabular} \end{figure}$	Figure 4: B-V-z color images of six galaxies representative of the six morphological classes used in this study. From top to bottom and left to right: spiral disks, Peculiar/Irregular, Peculiar/Tadpole, Peculiar/Merger, compact galaxies, and major mergers.
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$\begin{figure} \par\includegraphics[height=9cm]{9926fige.eps} \end{figure}$	Figure 5: Comparison between the morphological classification and the kinematical classification. Morphological classes are quoted in the bottom of X-coordinate, kinematical classes in Y-coordinate. RD refers to rotating disks, PR to perturbed rotations and CK to complex kinematics.
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$\begin{figure} \par\includegraphics[height=6cm]{9926figf.eps} \includegraphics[height=6cm]{9926figg.eps} \end{figure}$	Figure 6: top: $\log(A)-\log(C)$ diagram. Bottom: Gini-M20 diagram. Different symbols refer to the morphological classes: spiral disks are represented as blue circles, peculiars as green squares, compact galaxies as black diamonds, and mergers as red triangles.
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$\begin{figure} \par\begin{tabular}{c} \includegraphics[height=9cm]{9926figj.eps} \end{tabular} \end{figure}$	Figure 9: B₄₃₅-z₈₅₀ ( top) and V₆₀₆-I₈₁₄ ( bottom) observed color of the bulges for the rotating spiral disks sub-sample. The different evolutionary models are the same as in Fig. 8. Error bars are used to show the maximal pixel-by-pixel color range within each bulge.
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$\begin{figure} \par\includegraphics[height=3.3cm]{9926figm.eps} \end{figure}$	Figure 11: Ratio between stellar mass and SFR $_{\rm tot}$ as a function of galaxy radius. SFR $_{\rm tot}$ is defined as the sum of SFR $_{\rm UV}$ and SFR $_{\rm IR}$ . Only galaxies which have been detected by Spitzer are used in this analysis. The vertical line is at 1/3.2 of $R_{\rm max}$ which roughly corresponds to the disk scale length limit.
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$\begin{figure} \par\includegraphics[height=20.5cm]{9926fign.eps} \end{figure}$	Figure 12: F850LP/ F814W image, color map. Explanations are given at the end of this figure. Rotating spiral disks are marked with an asterisk near their name.
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$\begin{figure} \par\includegraphics[height=20.5cm]{9926figo.eps} \end{figure}$	Figure 12: continued.
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