------------------------------------------------------------------------
 gcoh.tex A&A 403, 1011 (2003)
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% A&A 403, 1011 (2003)
\documentstyle[apjfonts, emulateapj]{article}
\begin{document}
\title{18-cm VLA observations of OH towards the Galactic
Centre. Absorption and emission in the four ground-state OH lines}
\author{R. Karlsson\altaffilmark{1}, L. O. Sjouwerman\altaffilmark{2},
Aa. Sandqvist\altaffilmark{1}, J. B. Whiteoak\altaffilmark{3}}

Stockholm,
  Sweden (rolandk, aage@astro.su.se)}
\altaffiltext{2}{NRAO Array Operations Center, P.O.Box 0, Socorro NM
87801,
  USA (lsjouwer@aoc.nrao.edu)}
\altaffiltext{3}{CSIRO, Australian Telescope National Facility, Box 76,
Epping
  NSW 2121, Australia (jwhiteoa@atnf.csiro.au)}

\begin{abstract}
The OH distribution in the Sgr A Complex has been observed in the
1612-, 1665-, 1667- and 1720-MHz OH transitions with the Very Large Array
(VLA) in BnA configuration. Maps are presented
with a channel velocity resolution of about 9 km\,s$^{-1}$\ and with
angular
resolutions of 4$''$ $\times$ 3$''$. Some clear results are
highlighted here, such as absorption from the Circumnuclear Disk
(CND) and the OH-Streamer inside the CND near Sgr A$^*$, strong
absorption towards most of the eastern and western parts of the
Sgr A East shell, lack of absorption towards both Sgr A West and the
compact HII-regions to the east of Sgr A East, and double-lobed
structure of the High Negative Velocity Gas (HNVG)
oriented northeast and southwest of Sgr A$^*$, and finally compact,
point-like maser emission in all four transitions, in particular a
1720-MHz maser at $-$132km\,s$^{-1}$\ in the CND as counterpart to a
1720-MHz maser at $+$132km\,s$^{-1}$\ in the CND.
\end{abstract}

\end{document}
saerimner[262]:papfi> more GC
GCNEWSoh.tex   GCNEWSoh.tex~
saerimner[262]:papfi> more GCNEWSoh.tex
% A&A 403, 1011 (2003)
\documentstyle[apjfonts, emulateapj]{article}
\begin{document}
\title{18-cm VLA observations of OH towards the Galactic
Centre. Absorption and emission in the four ground-state OH lines}
\author{R. Karlsson\altaffilmark{1}, L. O. Sjouwerman\altaffilmark{2},
Aa. Sandqvist\altaffilmark{1}, J. B. Whiteoak\altaffilmark{3}}

\altaffiltext{1}{Stockholm Observatory, SCFAB-AlbaNova, SE-106 91
Stockholm,
  Sweden (rolandk, aage@astro.su.se)}
\altaffiltext{2}{NRAO Array Operations Center, P.O.Box 0, Socorro NM
87801,
  USA (lsjouwer@aoc.nrao.edu)}
\altaffiltext{3}{CSIRO, Australian Telescope National Facility, Box 76,
Epping
  NSW 2121, Australia (jwhiteoa@atnf.csiro.au)}

\begin{abstract}
The OH distribution in the Sgr A Complex has been observed in the
1612-, 1665-, 1667- and 1720-MHz OH transitions with the Very Large Array
(VLA) in BnA configuration. Maps are presented
with a channel velocity resolution of about 9 km\,s$^{-1}$\ and with
angular
resolutions of 4$''$ $\times$ 3$''$. Some clear results are
highlighted here, such as absorption from the Circumnuclear Disk
(CND) and the OH-Streamer inside the CND near Sgr A$^*$, strong
absorption towards most of the eastern and western parts of the
Sgr A East shell, lack of absorption towards both Sgr A West and the
compact HII-regions to the east of Sgr A East, and double-lobed
structure of the High Negative Velocity Gas (HNVG)
oriented northeast and southwest of Sgr A$^*$, and finally compact,
point-like maser emission in all four transitions, in particular a
1720-MHz maser at $-$132km\,s$^{-1}$\ in the CND as counterpart to a
1720-MHz maser at $+$132km\,s$^{-1}$\ in the CND.
\end{abstract}

\end{document}


--------------------------------------------------------------
Aage Sandqvist                       Tel. +46-8-55378511
Stockholm Observatory		     Fax. +46-8-55378510
SCFAB-AlbaNova
SE-106 91 Stockholm                  email: aage@astro.su.se
Sweden
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