\section{Thesis Project}

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\begin{frame}\frametitle{Thesis Project}

\textbf{The qualifier project did not include:}

\begin{itemize}
\item dark matter
\item super-massive black holes
\item gas dynamics
\item AGN feedback
\item star formation and death
\item a realistic treatment of dust extinction
\item spheroids of realistic mass and size
\item measurements of \sig\ consistent with observational technique
\end{itemize}

\end{frame}

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\begin{frame}\frametitle{Thesis Project}

\textbf{The thesis project will\ldots}

\begin{itemize}
 \item use \textbf{GADGET-2} to perform high-resolution dissipational simulations of galaxies including all of the major components missing from the qualifier project.%gas dynamics, gas cooling/heating, BH accretion, AGN feedback, stellar formation and death, supernova feedback. 
 \item use \textbf{Sunrise} to realistically treat dust extinction, create galaxy spectra, and perform simulated observations of galaxies.\pause
 \item use observational analysis tools to analyze images and spectra created by Sunrise.
\end{itemize}

\end{frame}

%----------------------

\subsection{High-resolution dissipational simulations}

\begin{frame}\frametitle{GADGET-2}

\textbf{GADGET-2:}

\begin{itemize}
\item Highly scalable simulation code written in C, parallelized with MPI.
\item Computes gravitational forces using Barnes-Hut tree method (or PM method, if desired).
\item Gas / ISM is handled using smoothed-particle hydrodynamics (SPH).
\item Gas cooling and heating are included.
\item Metallicity of ISM and star particles is tracked.
\end{itemize}

\end{frame}
%----------------------

\begin{frame}\frametitle{GADGET-2}

\begin{itemize}
\item New star particles are created from SPH particles stochastically based on the ISM density and temperature temperature, at a rate motivated by the Kennicutt-Schmidt law.
\item ISM metalicity increases in regions surrounding star formation.
\item Stars die: SN feedback heats and pressurizes the ISM. 
\item Accretion onto black hole and resulting feedback can be modeled in several ways\ldots 
\end{itemize}

\end{frame}
%----------------------

\begin{frame}\frametitle{GADGET-2}

\textbf{Method 1:} Spherical accretion; thermal feedback

\begin{itemize}
 \item Accretion occurs at Bondi-Hoyle-Lyttleton rate (limited by $\dot M_{Edd}$).
 \item Some of the accreted mass-energy ($10\%$) is converted to $L_{AGN}$.
 \item A small fraction of AGN luminosity ($0.5\%$) couples thermally to ISM.
\end{itemize}

 \pause 
\textbf{Method 2:} Non-spherical accretion; momentum feedback

\begin{itemize}
 \item Accretion occurs as gas (viscously) loses angular momentum (limited by $\dot M_{Edd}$).
 \item A fraction of the accreted mass-energy is converted to $L_{AGN}$.
 \item A fraction of the mass-energy couples back to the ISM through momentum transfer.
\end{itemize}

\end{frame}
%----------------------



\subsection{Simulated Observations}

\begin{frame}\frametitle{Sunrise}

\begin{itemize}
\item A polychromatic, Monte Carlo, radiative transfer code written in C++ and CUDA, parallelized with pthreads.
\item Requires shared memory machine with $\gtrsim 32$ GB of RAM.\pause
\item Main Input:
\begin{itemize}
 \item GADGET-2 Snapshot
 \item choice of dust grain model (MW, SMC, LMC, custom)
 \item camera information (positions, resolution)
\end{itemize}
\pause
\item Output: Images and spectra from a collection of virtual cameras.
\begin{itemize}
\item Images of galaxy
\item Doppler shifted spectra of galaxy (each pixel of each image contains a spectrum).
\end{itemize}

\end{itemize}

\end{frame}

%----------------------

\subsection{Simulated Observations}

\begin{frame}\frametitle{Sunrise}

\textbf{Basic steps:}

\begin{enumerate}
 \item Discretize spatial domain of simulation using adaptive mesh based on distribution of stars and gas.\pause
 \item Assume that the ISM dust content is proportional to the metallicity of ISM. \pause
 \item Stellar spectra are based on ages and metallicities (Starburst99 population synthesis model).\pause
 \item Stars younger than 10 Myr are assumed to be star forming region with enhanced dust and PDR; they are modeled using the MappingsIII code (Groves et al., 2008).
 \item Shoots $\sim10^6 - 10^7$ photon bundles from stars through the galaxy.
\end{enumerate}


\end{frame}

%----------------------

\subsection{Collision Analysis}

\begin{frame}\frametitle{Collision Analysis}

Perform a suite of galaxy collisions using GADGET-2\ldots

\begin{itemize}
\item Save GADGET-2 snapshots at $\leq 50$ Myr intervals.\pause
\item Analyse velocity dispersion using the standard (mass-weighted) method.\pause
\item For a subset of collisions, run Sunrise to create images and \sig.\pause
\item Compute flux-weighted \sig\ from spectra and compare with mass-weighted spectra.\pause
\item Analyze morphologies (concentration, gini coefficient, asymmetry), colors, and color excesses of systems.\pause
\item Look for correlations between morph, color, color excess, and the behavior of \sig\ in analogy with Lotz et al.
\end{itemize}

\end{frame}

%----------------------

\subsection{Research Plan}

\begin{frame}\frametitle{Trials}

\begin{itemize}
\item Select configurations for comparison with Johansson et al. and Lotz et al.
\item Select broad range of other collisions to mimic the range of collisions observed in nature. Vary:
\begin{itemize}
 \item gas fraction
 \item mass ratio
 \item Hubble type
 \item orbital parameters: pro vs. retrograde, apsidal distance, relative velocities
\end{itemize}
\item examine resolution effects (vary $N$, $h$, $\epsilon$)
\item test the influence of the dust model on measured \sig.
\item evaluate the difference between momentum and thermal AGN feedback.
\end{itemize}

\end{frame}

%----------------------

\begin{frame}\frametitle{Further Analysis}

\textbf{Further Analysis:}

\begin{itemize}
 \item Use Cosmological galaxy merger statistics and the results above to predict the fraction of galaxies at a given redshift with relaxed \sig.
 \item Predict evolution and scatter of the observed \msig\ relation.
 \item Attempt to create a set of diagnostics based on morphology, colors, and color excesses to determine the state of the measured and ``real'' \sig\ for an observed galaxy. 
\end{itemize}

\end{frame}

%----------------------

\begin{frame}\frametitle{Research Plan/Schedule}

\begin{description}
 \item[Dec 2010]Build workstation and configure software.
 \item[Mar 2011]Finish running low-resolution GADGET-2 test simulations and analyze with Sunrise (for practice). Streamline the spectral and morphological analysis process (Automate as much as possible).
 \item[May 2011]Decide on official set of initial configurations and begin running high resolution simulations on supercomputer. Begin Sunrise analysis.
\item[Feb 2012] Finish high-resolution simulations and Sunrise analysis. Begin statistical analysis and writing thesis / publications.
\item[Sept 2012] Finish writing thesis and submitting main results for publication.
 \end{description}
 
\color{white}{\cite{*}}
\end{frame}

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