All Figures

$\begin{figure} \par\includegraphics[width=4.9cm,clip]{0784f01a.eps}\hspace*{2mm}... ...eps}\hspace*{2mm} \includegraphics[width=4.9cm,clip]{0784f01c.eps} \end{figure}$ Figure 1: Imitated HST/WFPC2 V₆₀₆-I₈₁₄ color maps for an elliptical galaxy at redshift 0.299 when the offsets between blue and red images are 0.0 pixel ( left panel), 0.15 pixel ( middle panel) and 0.30 pixel ( right panel). The color maps are 50 $\times$ 50 pixel. ( See the electronic edition for a color version of this figure.)
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In the text

$\begin{figure} \par\includegraphics[width=6.75cm,clip]{0784f02.eps} \end{figure}$ Figure 2: Systematic offsets between V₆₀₆ and I₈₁₄ images in 27 GSS fields. Solid circle is I₈₁₄ image and cross is V₆₀₆ image.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0784f03.eps} \end{figure}$ Figure 3: Position offset for 178 point/point-like sources between two aligned images. The offsets are in the coordinates of WF3 chip. The median value in X is 0.006 pixel and the median value in Y is 0.004 pixel.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=0.32\textwidth]{0784f04a.eps} \i... ...84f04b.eps} \includegraphics[width=0.32\textwidth]{0784f04c.eps} } \end{figure}$ Figure 4: Left panel: center offset of the bright sources ( $m_{814} \leq 22$ ) between blue (V₆₀₆ or B₄₅₀) and red (I₈₁₄) image as a function of their positions in WFPC2 WF chip, expressed as the distance from the chip center. Middle panel: histograms of the center offset for all bright sources and for our ISOCAM-detected galaxies. Right panel: center offset for the point/point-like sources. In this panel, the mean value of the offset is 0.117 pixel with $\sigma$ = 0.088 pixel.
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In the text

$\begin{figure} \par {\includegraphics[height=3.7cm,width=3.8cm,clip]{0784f05a.ep... ...{2mm} \includegraphics[height=3.7cm,width=4.45cm,clip]{0784f05d.eps}\end{figure}$ Figure 5: V₆₀₆, I₈₁₄, the color map S/N ratio, as well as color map images of elliptical galaxy 03.0037 at redshift 0.1730. ( See the electronic edition for a color version of this figure.)
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In the text

$\begin{figure} \par {\includegraphics[height=3.7cm,width=3.8cm,clip]{0784f06a.ep... ...{2mm} \includegraphics[height=3.7cm,width=4.45cm,clip]{0784f06d.eps}\end{figure}$ Figure 6: Same as in Fig. 5 for disk galaxy 03.0046 at redshift 0.5120. ( See the electronic edition for a color version of this figure.)
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In the text

$\begin{figure} \par {\includegraphics[height=3.7cm,width=3.8cm,clip]{0784f07a.ep... ...{2mm} \includegraphics[height=3.7cm,width=4.45cm,clip]{0784f07d.eps}\end{figure}$ Figure 7: Same as in Fig. 5 for merging system 03.1309 at redshift 0.6170. ( See the electronic edition for a color version of this figure.)
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0784f08.eps} \end{figure}$ Figure 8: Histogram of the IR luminosity for 36 distant LIRGs.
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In the text

$\begin{figure} \par\hspace*{-1.5mm}\includegraphics[width=7.55cm,clip]{0784f09a.eps}\vspace*{7mm} \includegraphics[width=7.4cm,clip]{0784f09b.eps} \end{figure}$ Figure 9: V₆₀₆-I₈₁₄ (top) and B₄₅₀-I₈₁₄ (bottom) observed colors for LIRGs as a function of redshift. Similar to Fig. 6 in Menanteau et al. (2001), four solar metallicity, formed at z = 5 galaxy models, including an Elliptical galaxy (single burst), S0 galaxy ( $\tau = 1$ Gyr), Sbc galaxy ( $\tau = 7$ Gyr), irregular galaxy (constant SFR) are present for a comparison. Almost all LIRGs are redder than Sbc galaxy.
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In the text

$\begin{figure} \par\includegraphics[height=0.20\textwidth,clip]{078401im.eps}\in... ...412im.eps}\includegraphics[height=0.20\textwidth,clip]{078412cm.eps}\end{figure}$ Figure 10: I₈₁₄ band and color map images of distant LIRGs. For each target, the name and redshift are labeled top-left and top-right in the I₈₁₄ image. The color bar ranges from -1 to 3 for the V₆₀₆-I₈₁₄ color map and 0 to 4 for the B₄₅₀-I₈₁₄ color map. The blank in I₈₁₄ image is due to the target imaged close to the chip border. The size of each image is 40 $\times$ 40 kpc except for the object 03.1309, which is 60 $\times$ 60 kpc to display the whole merging system. ( See the electronic edition for a color version of this figure.)
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In the text

$\begin{figure} \par\includegraphics[height=0.21\textwidth,clip]{078413im.eps}\in... ...424im.eps}\includegraphics[height=0.21\textwidth,clip]{078424cm.eps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[height=0.21\textwidth,clip]{078425im.eps}\in... ...436im.eps}\includegraphics[height=0.21\textwidth,clip]{078436cm.eps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0784f11.eps} \end{figure}$ Figure 11: Stellar mass versus time scale to duplicate the bulk of stars at a rate of the observed value. The stellar mass is derived from K band luminosity. The size of the point is scaled by the SFR. Nearby galaxies listed in Table 3 with available K band luminosity are shown with open circles for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0784f12.eps} \end{figure}$ Figure 12: Central surface brightness of the disk components as a function of redshift for LIRG disks in our sample (solid square), compared with the large disk galaxies in L98 (open circle). The long-dashed line is the selection criterion ( $I_{\rm AB}$ < 22.5) for a pure disk galaxy with scale length 4 h₅₀^-1 kpc.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0784f13.eps} \end{figure}$ Figure 13: Central color versus concentration index. The distributions (large crosses) of normal elliptical, Sab and Sbc galaxies are derived from a nearby galaxy sample (Frei et al. 1996). The modeling colors for the galaxies E, S0, Sbc and Irr at this redshift are 2.05, 1.88, 1.10 and 0.38 respectively (see Sect. 5.2.2). We assume that Sbc galaxies are bluer by 0.1 mag than E/S0 galaxies and Scd galaxies are 0.1 mag bluer than Sbc galaxies in the bulge color (de Jong 1996). A central color of 2.05 is adopted for E/S0 galaxies. The CFRS ID is labeled for each data point. A Spearman rank-order (S-R) correlation analysis reveals a correlation coefficient of -0.42 with a probability of 0.026 that the null hypothesis of no correlation is true.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{0784f14.ps} \end{figure}$ Figure A.1: The distribution function of Poisson noise at S/N = 2 and its Log-normal approximation (continuous line) for the same S/N ratio. Even at this low S/N the two functions differ by a value of 0.15 at most.

In the text

$\begin{figure} \par\includegraphics[width=4.9cm,clip]{0784f01a.eps}\hspace{2mm}... ...eps}\hspace{2mm} \includegraphics[width=4.9cm,clip]{0784f01c.eps} \end{figure}$	Figure 1: Imitated HST/WFPC2 V₆₀₆-I₈₁₄ color maps for an elliptical galaxy at redshift 0.299 when the offsets between blue and red images are 0.0 pixel ( left panel), 0.15 pixel ( middle panel) and 0.30 pixel ( right panel). The color maps are 50 $\times$ 50 pixel. ( See the electronic edition for a color version of this figure.)
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$\begin{figure} \par\includegraphics[width=6.75cm,clip]{0784f02.eps} \end{figure}$	Figure 2: Systematic offsets between V₆₀₆ and I₈₁₄ images in 27 GSS fields. Solid circle is I₈₁₄ image and cross is V₆₀₆ image.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0784f03.eps} \end{figure}$	Figure 3: Position offset for 178 point/point-like sources between two aligned images. The offsets are in the coordinates of WF3 chip. The median value in X is 0.006 pixel and the median value in Y is 0.004 pixel.
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$\begin{figure} \par {\includegraphics[height=3.7cm,width=3.8cm,clip]{0784f05a.ep... ...{2mm} \includegraphics[height=3.7cm,width=4.45cm,clip]{0784f05d.eps}\end{figure}$	Figure 5: V₆₀₆, I₈₁₄, the color map S/N ratio, as well as color map images of elliptical galaxy 03.0037 at redshift 0.1730. ( See the electronic edition for a color version of this figure.)
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$\begin{figure} \par {\includegraphics[height=3.7cm,width=3.8cm,clip]{0784f06a.ep... ...{2mm} \includegraphics[height=3.7cm,width=4.45cm,clip]{0784f06d.eps}\end{figure}$	Figure 6: Same as in Fig. 5 for disk galaxy 03.0046 at redshift 0.5120. ( See the electronic edition for a color version of this figure.)
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$\begin{figure} \par {\includegraphics[height=3.7cm,width=3.8cm,clip]{0784f07a.ep... ...{2mm} \includegraphics[height=3.7cm,width=4.45cm,clip]{0784f07d.eps}\end{figure}$	Figure 7: Same as in Fig. 5 for merging system 03.1309 at redshift 0.6170. ( See the electronic edition for a color version of this figure.)
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0784f08.eps} \end{figure}$	Figure 8: Histogram of the IR luminosity for 36 distant LIRGs.
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$\begin{figure} \par\includegraphics[height=0.21\textwidth,clip]{078413im.eps}\in... ...424im.eps}\includegraphics[height=0.21\textwidth,clip]{078424cm.eps}\end{figure}$	Figure 10: continued.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{0784f11.eps} \end{figure}$	Figure 11: Stellar mass versus time scale to duplicate the bulk of stars at a rate of the observed value. The stellar mass is derived from K band luminosity. The size of the point is scaled by the SFR. Nearby galaxies listed in Table 3 with available K band luminosity are shown with open circles for comparison.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0784f12.eps} \end{figure}$	Figure 12: Central surface brightness of the disk components as a function of redshift for LIRG disks in our sample (solid square), compared with the large disk galaxies in L98 (open circle). The long-dashed line is the selection criterion ( $I_{\rm AB}$ < 22.5) for a pure disk galaxy with scale length 4 h₅₀^-1 kpc.
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