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\begin{document}

\title{On the Optimal Inclusion of the Galactic Center in the VLA Sky Survey}


\author{Elisabeth Mills}
\affil{Affiliation not available}

  
\author{Adam Ginsburg}
\affil{Affiliation not available}
  



\date{\today}

\maketitle

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\begin{abstract}
Placeholder
\end{abstract}


\section{Introduction} 
Context for Galactic center (radio) studies

\section{Summary of Science Goals and Observing Strategies}

\begin{itemize}
\item Science Goals
\begin{enumerate}
\item The Galactic Center as a Unique Star Formation Environment
\item Probing the Stellar Populations in the Galactic Center
\item The Origins of Extreme Gas Properties in the Galactic Center
\item Large-scale Magnetic Field Strength and Geometry in the Galactic Center
\item Feeding the Gas Reservoir in the Galactic Center
\item Galactic Center Outflows from Small to Large Scales
\end{enumerate}
\item Requirements on Survey Design
\begin{enumerate}
\item Frequencies
\item Sensitivity
\item Resolution
\item Survey Area
\end{enumerate}
\item Observing Techniques
\begin{enumerate}
\item Molecular Lines
\item Continuum and Recombination Lines
\item Polarization
\end{enumerate}
\end{itemize}

\section{Science Goals}
Summary placeholder


\subsection{Magnetic Field}



\section{Survey Design}
Summary placeholder

\subsection{Frequencies}

We have identified the C-band (4-7 GHz) as the ideal range to perform a large-area survey of the central regions of our galaxy [NOTE: Can we come up with a term to identify "-3 to +3 degrees", CMZ+?].  

The key requirements of a large survey, from a practical perspective, are:
\begin{itemize}
\item Avoiding RFI - this rules out low frequencies ($<2$ GHz)
\item Field of view - in order to mosaic a region larger than a few square degrees, high frequencies with small primary beams cannot practically be used.
\item Velocity resolution & coverage - The EVLA can do this in any band [NOTE: leave out as a bullet]
\item Recombination line sensitivity - [NOTE: mixed bag - more RRLs per fractional bandwidth at lower frequencies, but they are fainter]
\item Sensitivity to nonthermal features
\item Choice of molecular tracers - CH3OH, H2CO.  Nothing better until you get to NH3, where beams are too small.
\item Synergy with existing surveys
\end{itemize}

Justification for multiple bands?
\begin{itemize}
\item Calculating Spectral indices
\item Excitation analysis of molecular lines
\end{itemize}

Optimizing the correlator to observe a wide continuum bandwidth, and resolve typical Galactic center linewidths




\subsection{Sensitivity}

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