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\@writefile{toc}{\contentsline {section}{\numberline {1}Introduction}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {2}Simulations}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.1}Simulated Images}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces A simulated image of Cluster C2 at $t=0.67$, color coded by $V$-band surface brightness, $\mu _V$. Black represents all luminosity at $\mu _V$$<26.0$ mag/arcsec$^2$. Each other color represents a bin of one mag/arcsec$^2$: red is $\mu _V$$=26.0-27.0$, orange is $\mu _V$$=27.0-28.0$, etc. This same color scheme will be used in all simulated images shown in this paper. The distance scale in the upper right indicates the length of one megaparsec in physical units. }}{11}}
\newlabel{fig:example}{{1}{11}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Evolution and Production of ICL}{12}}
\newlabel{sec:prodicl}{{3}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces The fraction of cluster luminosity contained in 1 mag/arcsec$^2$\ bins of $\mu _V$\ for each of the three clusters at three different timepoints in their evolution. }}{12}}
\newlabel{fig:rotlum}{{2}{12}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Evolution of ICL Luminosity}{13}}
\newlabel{sec:evicl}{{3.1}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces \emph  {Top}: The fraction of the luminosity in each cluster which is at ICL surface brightness ($\mu _V$$>26.5$ mag/arcsec$^2$) as a function of time ($f_{ICL}$). The top axis shows the corresponding nominal redshift. \emph  {Middle}: The fractional change in ICL luminosity per unit time as a function of time ($\Delta f_{ICL}$). \emph  {Bottom}: The running mean ($\mathaccent "775E\relax {\mu }$) with standard deviation ($\mathaccent "775E\relax {\sigma }$) error bars, using a running bin of ten time points, for the $\Delta f_{ICL}$\ function. The time is the average of the timepoints in each bin. }}{13}}
\newlabel{fig:delta}{{3}{13}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {3.1.1}Initial Evolution of Galaxies}{14}}
\newlabel{sec:initial}{{3.1.1}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces The $\Delta f_{ICL}$\ function at very early times for a single isolated galaxy (top), a small galaxy group (middle) and the entire cluster (bottom) for cluster C1. The structure of the $\Delta f_{ICL}$\ function for the cluster mimics that of the group. }}{14}}
\newlabel{fig:onegal}{{4}{14}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}Individual Clusters}{15}}
\newlabel{sec:clusters}{{3.2}{15}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {3.2.1}Cluster C1}{15}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Simulated images of the evolution of Cluster C1 color coded by $V$-band surface brightness, $\mu _V$. Black represents all luminosity at $\mu _V$$<26.0$ mag/arcsec$^2$. Each other color represents a bin of one mag/arcsec$^2$: red is $\mu _V$$=26.0-27.0$, orange is $\mu _V$$=27.0-28.0$, etc. The color scale is identical to that used in Figure 1{}{}{}\hbox {}. The distance scale in the upper left indicates the length of one megaparsec in physical units. }}{16}}
\newlabel{fig:c1}{{5}{16}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {3.2.2}Cluster C2}{17}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces Simulated images of the evolution of Cluster C2 color coded by $V$-band surface brightness, $\mu _V$. Black represents all luminosity at $\mu _V$$<26.0$ mag/arcsec$^2$. Each other color represents a bin of one mag/arcsec$^2$: red is $\mu _V$$=26.0-27.0$, orange is $\mu _V$$=27.0-28.0$, etc. The color scale is identical to that used in Figure 1{}{}{}\hbox {}. The distance scale in the upper left indicates the length of one megaparsec in physical units. }}{17}}
\newlabel{fig:c2}{{6}{17}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {3.2.3}Cluster C3}{18}}
\newlabel{sec:c3}{{3.2.3}{18}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Simulated images of the evolution of Cluster C3 color coded by $V$-band surface brightness, $\mu _V$. Black represents all luminosity at $\mu _V$$<26.0$ mag/arcsec$^2$. Each other color represents a bin of one mag/arcsec$^2$: red is $\mu _V$$=26.0-27.0$, orange is $\mu _V$$=27.0-28.0$, etc. The color scale is identical to that used in Figure 1{}{}{}\hbox {}. The distance scale in the upper left indicates the length of one megaparsec in physical units. }}{18}}
\newlabel{fig:c3}{{7}{18}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {3.2.4}Increased Time Resolution of an Accretion Event}{19}}
\newlabel{sec:hires}{{3.2.4}{19}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces Simulated images of a short section of the evolution C2 at high time resolution color coded by $V$-band surface brightness, $\mu _V$. Black represents all luminosity at $\mu _V$$<26.0$ mag/arcsec$^2$. Each other color represents a bin of one mag/arcsec$^2$: red is $\mu _V$$=26.0-27.0$, orange is $\mu _V$$=27.0-28.0$, etc. The color scale is identical to that used in Figure 1{}{}{}\hbox {}. The distance scale in the upper left indicates the length of one megaparsec in physical units. The arrow points to the small galaxy group which moves through the cluster core (see Section 3.2.4{}{}{}\hbox {} for details). }}{19}}
\newlabel{fig:hires}{{8}{19}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.3}Evolution of Very Faint ICL ($\mu _V$$>30.0$)}{20}}
\newlabel{sec:ficl}{{3.3}{20}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces The $f_{ICL}$\ and $\Delta f_{ICL}$\ plots for C2. The bold section indicates the section used in the high time resolution analysis of \S  3.2.4{}{}{}\hbox {}. }}{20}}
\newlabel{fig:hires_plot}{{9}{20}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.4}ICL Morphology}{22}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.5}Radial Distribution of ICL in Evolved Clusters}{23}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Summary}{24}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces \emph  {Top}: The $\Delta f_{ICL}$\ function for each cluster (closed circles) and the $\Delta f_{FICL}$\ function (open squares) which is simply the $\Delta f_{ICL}$\ function for luminosity at $\mu _V$$>30.0$. The curves follow a third order polynomial fit to the data. The colored curves are those sections of the $\Delta f_{FICL}$\ which are highly correlated with sections of the $\Delta f_{ICL}$. \emph  {Middle Top}: The $\Delta f_{ICL}$\ function, with the highly correlated segments of the $\Delta f_{FICL}$\ function shifted in time by $\Delta t_{max}$. \emph  {Middle Bottom}: $\Delta t_{max}$, or the time shift which results in the highest correlation, for the highly correlated segments of the $\Delta f_{FICL}$\ function. \emph  {Bottom}: The highest value of the correlation coefficient, $r$, for each bin of the $\Delta f_{FICL}$\ function resulting from shifting $\Delta f_{FICL}$\ backward in time by $\Delta t < 0.1$. }}{28}}
\newlabel{fig:faint}{{10}{28}}
\@writefile{lof}{\contentsline {figure}{\numberline {11}{\ignorespaces The fraction of ICL luminosity as a function of projected radius in each of the three simulated clusters. }}{28}}
\newlabel{fig:iclfrac}{{11}{28}}
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