------------------------------------------------------------------------
From: Michael Burton  mgb@phys.unsw.edu.au 
To: gcnews@zia.aoc.nrao.edu
Subject: submit burton_eyepaper.tex MN, submitted.

%astro-ph/0308262

\documentstyle{article}

\newcommand{\lsol}{\hbox{$\rm L_\odot$}}
\newcommand{\msol}{\hbox{\,$\rm M_\odot$}}
\newcommand{\e}[1]{$10^{#1}$}
\newcommand{\ee}[1]{$\times 10^{#1}$}         
\newcommand{\kms}{~km\,s$^{-1}$} 
\newcommand{\cm}[1]{~cm$^{#1}$}
\newcommand{\microm}{\,$\mu$m}
\newcommand{\VLSR}{V$_{\rm LSR}$}

\newcommand{\co}{$^{12}$CO}    
\newcommand{\oh}{OH(1720 MHz)}

\newcommand{\brg}{Br\,${\gamma}$}
\newcommand{\hei}{He\,{\sc i}}
\newcommand{\h}{H$_2$}
\newcommand{\hi}{H\,{\sc i}}
\newcommand{\hr}{H\,{\sc ii}}

\begin{document}


\title{The Eye of the Tornado---an isolated, high mass young stellar object
near the Galactic centre}

\author{M. G. Burton$^1$, J. S. Lazendic$^{2,3}$, F. Yusef-Zadeh$^{4}$,
       M. Wardle$^5$ \\ \normalsize $^1$ School of Physics, University
       of New South Wales, Sydney NSW 2052, Australia\\ \normalsize
       $^2$ School of Physics A28, University of Sydney, Sydney NSW
       2006, Australia\\ \normalsize $^3$ Australia Telescope National
       Facility, CSIRO, PO Box 76, Epping NSW 1710, Australia \\
       \normalsize $^4$ Department of Physics and Astronomy,
       Northwestern University, Evanston, IL 60208, USA \\ \normalsize
       $^5$ Department of Physics, Macquarie University, Sydney, NSW
       2019, Australia}

\maketitle

\begin{abstract}
We present infrared (AAT, UKIRT) and radio (VLA, SEST) observations of
the Eye of the Tornado, a compact source apparently near the head of
the Tornado Nebula. The near-infrared
\brg\ and \hei\ lines are broad (FWHM $40$ and $30$\,\kms, respectively) 
and have a line centre at V$_{\rm LSR} \sim -$205\kms.  This
corresponds to a feature at the same velocity in the $\rm
^{12}CO$\,J=1--0 line profile.  The kinematic velocity derived from
Galactic rotation places the Eye at the distance of the Galactic
Centre (i.e.\ 8.5\,kpc) and separated (probably foreground) from the
Tornado Nebula. Four knots of emission are seen in the \brg\ line and
at 6 and 20\,cm.  Together with the flat radio spectral index, we
confirm that the Eye contains ionized gas, but that this is embedded
within a dense molecular core.  The spectral energy distribution can
be modelled as a two-component blackbody + greybody, peaking at far--IR
wavelengths. The knots are UC \hr\ regions, and the core contains a
luminous ($\sim 2 \times 10^4$\,\lsol), embedded, massive young
stellar source.  We also propose a geometrical model for the Eye to
account for both its spectral energy distribution and its morphology.
\end{abstract}




\end{document}