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%  (symbolsRL.tex; short version: Jan.96; R.Liseau)
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%  Journals and references 
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%  Units
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\begin{document}

First detection of the \nhthree\,($J, \,K = 1,0\rightarrow 0,0$) 572.5\,GHz
line from a dark cloud
 
\normalsize
\section{Introduction}

Already from early molecular line work it was clear that \ro\,A 
is a particularly dense core in the star forming \roc\ 
(Loren et al. 19XX, Wilking \& Lada 19XX). The 
spectacular Class\,0 source VLA\,1623 at its southern tip is
believed to be extremely young (Andr\'e et al. 19XX), driving 
a highly collimated molecular outflow (Dent et al. 19XX).  


\section{Observations and data reductions}

The observations of \ro\,A in the 572.5\,GHz line of \nh3\ were 
performed with Odin, a Swedish-international satellite (Canada, 
Finland, France) for aeronomy and astronomy. The satellite and
its payload have been reviewed by (references...).

At the frequency of the \nhthree\,(1,0-0,0) line, 572.49XXXX\,GHz, 
the beam of the 1.1\,m telescope is 120\asec, confirmed by 
observations of the planet Jupiter. Further, the pointing accuracy 
has been determined to be better than 15\asec\ and the main beam 
efficiency to be 95\%.

A three point 
strip scan was made along position angle 68\adeg, centered on 
\radot{16}{26}{24}{9}, \decdms{-24}{23}{44} (J2000) and with
relative offsets of 45\asec. The southwest position is coincident
with the bright CO\,(3-2) knot in the red outflow (Dent et al. 19XX)
and the northeast position is that of CS\,(5-4) maximum emission 
(Liseau, unpublished SEST data). 
 
The front-end is a cooled (120\,K) Schottky receiver and
observations were obtained in Dicke-switched mode, with total
integration times per position of XXXX seconds. In addition, a
XXXX\,s observation was made toward an OFF position 1\adeg\ north
of the source. 

Tunable over a range of 17\,GHz, the instantaneous bandwidth 
is 1\,GHz. The 10000 channels of the Acousto Optical Spectrometer
(AOS) had a selected width of XXkHz (0.32\,\kms).
The 572\,Ghz receiver was known not to be phase locked, but 
reasonably well tuned in frequency. The frequency stability of 
the receiver was monitored using the telluric ozone line at 
XXXX\,GHz (Fig.\ref{ozone.ps}). This established that during the 
observations of \ro\,A the frequency drift was at most one channel,
allowing the individual scans to be co-added into a total average.


\section{Results}



\section{Discussion}


\section{Conclusions}
\end{document}