formatting edits

Author: Amy Roberts

chapter1.tex

@@ -94,8 +94,9 @@ \subsection{Neutrino Oscillation}
 ,
 \end{multline}
 where $c_{ij} = \cos{\theta_{ij}}$ and $s_{ij} = \sin{\theta_{ij}}$, $\delta$ is the Dirac CP-violating phase, and the Majorana CP-violating phases $\alpha_{ij}$ are only relevant if the neutrino is a Majorana fermion as discussed in {\sect}~\ref{sec:mass}.  Several generations of long-baseline neutrino experiments using solar, atmospheric, and reactor neutrinos have impressively constrained the mixing parameters and mass differences.  A summary of the parameters is given in {\tab}~\ref{tab:neutrinoParameters}.
-\begin{table*}
+\begin{table}
 \centering
+\caption[\uppercase{Neutrino oscillation parameters}]{\uppercase{Neutrino oscillation parameters} \label{tab:neutrinoParameters}}
 \begin{tabular}{lll}\toprule
 Parameter & Best Fit ($\pm$ 1$\sigma$) & 3$\sigma$ \\
 \midrule
@@ -106,9 +107,11 @@ \subsection{Neutrino Oscillation}
 $\sin^2{\theta_{13}}$ & $0.025^{+0.007}_{-0.008}$ & 0.005 - 0.050 \\   
 \bottomrule  
 \end{tabular}
-\caption[Neutrino oscillation parameters.]{Three-neutrino oscillation parameters, determined by a global fit to relevant neutrino data.   The mixing angles $\sin^2{\theta_{12}}$ and $\sin^2{\theta_{13}}$ were determined using reactor $\overline{\nu}_e$ spectra calculated in {\refref}~\citep{reactorNeutrinoSpectrum}.  Note that while it is known that $m_1 < m_2$, the sign of ${\Delta}m^2_{31}$ is not known.  The table is from {\refref}~\citep{PDG}.}
-\label{tab:neutrinoParameters}
-\end{table*}
+\begin{flushleft}
+\small $\quad\,$NOTE: 
+Three-neutrino oscillation parameters, determined by a global fit to relevant neutrino data.   The mixing angles $\sin^2{\theta_{12}}$ and $\sin^2{\theta_{13}}$ were determined using reactor $\overline{\nu}_e$ spectra calculated in {\refref}~\citep{reactorNeutrinoSpectrum}.  Note that while it is known that $m_1 < m_2$, the sign of ${\Delta}m^2_{31}$ is not known.  The table is from {\refref}~\citep{PDG}.
+\end{flushleft}
+\end{table}
 It is significant that the absolute values of the mass differences are measured; the ordering of the mass eigenstates is unknown.  Three different ``mass heierarchies'' are possible: the normal heierarchy (NH) where $m_1 < m_2 < m_3$, the inverted heierarchy (IH) where $m_3 < m_1 < m_2$, and the quasi-degenerate heierarchy (QD) where the mass scale is close to the current limit so that $m_1 \approx m_2 \approx m_3$.  A diagram of the three mass heierarchies is shown in {\fig}~\ref{fig:massScale}.
 \begin{figure}[htp]
 \centering

chapter2.tex

@@ -113,7 +113,7 @@ \subsection{NME calculations and valence States}
 \end{figure}
 The single-particle energy levels were adjusted in the QRPA calculation \citep{SuhonenEnergyAdjust} to provide better agreement with the data.  These changes reduced the QRPA calculation of \NME by approximately a factor of two, bringing it into agreement with the shell-model calculation of \NME.  This reduction in the spread of calculated \NME is particularly valuable to reducing the uncertainty of mass limits or estimates from \zvbb searches. 
 
-\section{Nucleon-nucleon correlations and the impact they have on NME}
+\section{Nucleon-Nucleon Correlations and the Impact they have on \NME}
 \label{sec:correlations}
 \begin{comment}
 \begin{itemize}

chapter5.tex

@@ -429,7 +429,7 @@ \section{Placing a Limit on Excited \zp States}
 % excitation energy, not timing
 % don't show past big peak
 
-\section{Fitting the \zp ground state}
+\section{Fitting the \zp Ground State}
 \label{sec:DWBA}
 \begin{comment}
 DWBA calculation