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From: satofm@u-gakugei.ac.jp (SATO Fumio)
X-Sender: satofm@pop.u-gakugei.ac.jp
Subject: submit sgrbpaper.tex to appear in ApJ, May 2000
Cc: satofm@u-gakugei.ac.jp
MIME-Version: 1.0


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\begin{document}

%% Between these brackets you write the title of your paper:
\title{{Cloud Collision-Induced Star Formation in Sagittarius B2. I. 
Large-Scale Kinematics}}

%% Here comes the author(s) of the paper, please indicate within $^...$
%% the number which corresponds to the institute of each author.
\author{ Fumio SATO$^{1, 2}$, Tetsuo HASEGAWA$^3$, John B. WHITEOAK$^4$ \ and
Ryosuke MIYAWAKI$^5$ }

%% Here you write your institute name(s) and address(es),
%% the number in $^..$ indicates your author number, for example:
\institute{ $^1$ {Department of Astronomy and Earth Sciences, Tokyo Gakugei
     University, Koganei, Tokyo 184-8501, Japan} \\
$^2$ {Institut d'Astrophysique Spatiale, Batiment 121, Universite
Paris-Sud, 91405
     Orsay cedex, France} \\
$^3$ {Institute of Astronomy, The University of Tokyo, Osawa, Mitaka,
     Tokyo 181-8588, Japan} \\
$^4$ {Australia Telescope National Facility, CSIRO, PO Box 76, Epping,
     NSW 1710, Australia} \\
$^5$ {Department of Science Education, Fukuoka University of Education,
     Munakata, Fukuoka 811-4192, Japan} \\
}

%% Here you may write the e-mail address of one or more of the authors
%% who will act as contact person for preprint requests etc, for example:
{E-mail contact: satofm@u-gakugei.ac.jp}


%% IF YOU USE ANY PERSONAL LATEX COMMANDS IN YOUR ABSTRACT,
%% PLEASE INCLUDE THEIR DEFINITIONS HERE!


%% Within the following brackets you place your text:
\begin{abstract}
{We present maps of a $\sim$14 pc $\times$ 20 pc region covering the Sgr B2
molecular cloud complex in the $^{13}$CO (1 -- 0) and CS (1 -- 0) lines
with high angular resolution.   A more restricted central area was also
mapped in the C$^{18}$O (1 -- 0) line.   The $^{13}$CO cloud consists of
two components: a compact core of $\sim$3 pc in diameter roughly centered
on Sgr B2 (M) and an extended plateau of $\sim$17 pc $\times$ 7.5 pc area
containing the maser sources and most of the HII regions.   Compact,
massive ($\sim$3 $\times$ $10^{5}$ $M_{\odot}$) C$^{18}$O cores are
associated with Sgr B2(M) and Sgr B2(N).   The obtained intensity
distributions are compared with those of molecular masers and compact HII
regions reported in the literature.   Low-velocity (40 -- 65 km s$^{-1}$)
masers, with positions roughly aligned in the north--south line connecting
the three major compact HII region complexes, are located near the eastern
margin of a large hole in the low-velocity molecular cloud.   In contrast,
most of the high-velocity (65 -- 80 km s$^{-1}$) masers are distributed
near the center of a compact molecular cloud at higher velocity, where a
shock seems to have occurred.   These results provide further evidence
supporting the cloud--cloud collision hypothesis based on limited $^{13}$CO
(1 -- 0) data (Hasegawa et al. 1994).   In addition, this hypothesis
appears to be consistent with a wide range of new observations that have
appeared in the literature.}
\end{abstract}
% Here you write which journal accepted your paper, for example:
{ To appear in Astrophys. J., 534, No.2 (May 10, 2000) }



\end{document}

******************************
SATO Fumio
Tokyo Gakugei University
Dept. of Astronomy & Earth Sciences
Koganei, Tokyo 184-8501, Japan
Tel:  +81 42 329 7528
Fax:  +81 42 329 7538
satofm@u-gakugei.ac.jp
******************************


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