All Figures

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5737fig1.ps} \end{figure}$ Figure 1: The histogram of the redshift and the absolute B band magnitude distribution for our LCG sample.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5737fig2.ps} \end{figure}$ Figure 2: F850LP magnitudes and half light radii (R_1/2) of our 39 LCGs shown in comparison with the completeness curves of the GOODS survey as depicted on the magnitude-size plane. The percentage completeness is marked on the individual curves. The completeness curves are plotted in intervals of 10% and were kindly provided by Harry Ferguson.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{5737fig3.ps} \end{figure}$ Figure 3: The variation of half-light radius(in units of ACS pixels) of stars with RA and Dec across the GOODS-S field in the F850LP filter. This plot uses $\sim$ 60 stars spread across the field.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.6cm,clip]{5737fig4.ps} \end{figure}$ Figure 4: The histogram of the difference between the B/T ratios obtained by using the nearest and the 2nd nearest star to the galaxy as the PSF.
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In the text

$\begin{figure} \par\hspace*{-5mm}\includegraphics[width=3.8cm,clip]{5737fg5a.ps}... ...c.ps}\hspace*{4.5mm} \includegraphics[width=4.4cm,clip]{5737fg5d.ps}\end{figure}$ Figure 5: From top-left to bottom-right 30 $\times$ $30~{\rm kpc}$ F850LP image, Galfit Model image, Residual image and the B-z color map of the LCG 905632. North is up, East is to the left. The galaxy name, redshift and morphological classification are indicated in the F850LP galaxy image. The horizontal bar at the bottom right of the galaxy image indicates $1\hbox {$^{\prime \prime }$ }$ . The intensity scaling is the same (squareroot) in each of the three grayscale images.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5737fig6.ps} \end{figure}$ Figure 6: A comparison of the azimuthally averaged F850LP band radial surface brightness profile of the galaxy 905632 (points with error bars), as compared to the surface brightness profile of the model image produced by galfit (red smooth line) produced using the IRAF task ELLIPSE.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5737fig7.ps} \end{figure}$ Figure 7: B-z observed color vs redshift evolution for three, Solar metallicity, formed at redshift = 5.0 spectrophotometric galaxy models assuming instantaneous burst (early type), exponentially decaying SFR with an e-folding time scale of 1 Gyr (S0) and 7 Gyr (late type). A young starburst has also been plotted for comparison, assuming a power law spectra $L_{\nu } \propto \nu ^{-1}$ . Our sample LCGs are plotted using different symbols for different morphological class, with Early types (E) as red open circles, S0 as black diagonal crosses, Disk dominated (S) as blue stars, Irr/Tadpole as blue open triangles and Mergers (M1/M2) as blue filled squares.
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In the text

$\begin{figure} \par\includegraphics[width=3.35cm,clip]{5737f801.eps}\hspace*{4mm... ...3.eps}\hspace*{4mm} \includegraphics[width=3.9cm,clip]{5737f824.eps}\end{figure}$ Figure 8: F850LP and the B-z color map images. For each target, the name and redshift are labeled at the top-left and top-right in the F850LP image. Our morphological classification is indicated at the bottom-left of each image. The size of each image is 30 $\times$ 30 kpc and the bar at the bottom-right of each image indicates 1.0 $^{\prime \prime }$ . North is up, East is to the left. The intensity scaling is the same (squareroot) in all the grayscale images, while the dynamic range is different for different objects owing to the fact that the max or central intensity can be different for different objects. The color bar shows the B-z color range from 0 to 4 except for object ID 904604, 907361 and 909015 where it ranges from 0 to 6. The blank in object ID 907305 is due to imaging at the edge of the GOODS CDFS region.
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In the text

$\begin{figure} \par\includegraphics[width=3.35cm,clip]{5737f825.eps}\hspace*{4mm... ...eps}\hspace*{4mm} \includegraphics[width=3.9cm,clip]{5737f848.eps} \end{figure}$ Figure 8: continued.
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In the text

$\begin{figure} \par\includegraphics[width=3.35cm,clip]{5737f849.eps}\hspace*{4mm... ...eps}\hspace*{4mm} \includegraphics[width=3.9cm,clip]{5737f872.eps} \end{figure}$ Figure 8: continued.
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In the text

$\begin{figure} \par\includegraphics[width=3.35cm,clip]{5737f873.eps}\hspace*{4mm... ...} \includegraphics[width=3.9cm,clip]{5737f878.eps}\hspace*{4.2cm}}\end{figure}$ Figure 8: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{5737fig9.ps}\end{figure}$ Figure A.1: $K_{\rm s}$ band number counts for the VLT GOODS/EIS.

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{5737fg10.ps}\end{figure}$ Figure B.1: Variation of half light radius R_1/2 of the PSF stars (in the F850LP filter) used by us against the B-z color of the PSF stars. Different symbols have been used for faint ( $m_z \geq 18.5$ ) and bright ( $m_z \leq 18.5$ ) stars using an arbitrary definition of what constitutes a bright star. Notice that at a given color, the brighter stars tend to have larger R_1/2 (even though there is a considerable amount of scatter).

In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5737fig1.ps} \end{figure}$	Figure 1: The histogram of the redshift and the absolute B band magnitude distribution for our LCG sample.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5737fig2.ps} \end{figure}$	Figure 2: F850LP magnitudes and half light radii (R_1/2) of our 39 LCGs shown in comparison with the completeness curves of the GOODS survey as depicted on the magnitude-size plane. The percentage completeness is marked on the individual curves. The completeness curves are plotted in intervals of 10% and were kindly provided by Harry Ferguson.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{5737fig3.ps} \end{figure}$	Figure 3: The variation of half-light radius(in units of ACS pixels) of stars with RA and Dec across the GOODS-S field in the F850LP filter. This plot uses $\sim$ 60 stars spread across the field.
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$\begin{figure} \par\includegraphics[angle=270,width=8.6cm,clip]{5737fig4.ps} \end{figure}$	Figure 4: The histogram of the difference between the B/T ratios obtained by using the nearest and the 2nd nearest star to the galaxy as the PSF.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5737fig6.ps} \end{figure}$	Figure 6: A comparison of the azimuthally averaged F850LP band radial surface brightness profile of the galaxy 905632 (points with error bars), as compared to the surface brightness profile of the model image produced by galfit (red smooth line) produced using the IRAF task ELLIPSE.
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$\begin{figure} \par\includegraphics[width=3.35cm,clip]{5737f825.eps}\hspace{4mm... ...eps}\hspace{4mm} \includegraphics[width=3.9cm,clip]{5737f848.eps} \end{figure}$	Figure 8: continued.
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