Molecular Gas in the Galactic Center Region
I. Data from a Large Scale C18O(J = 1 -> 0) Survey
G. Dahmen(1,4), S. Hüttemeister(2,1,5), T.L. Wilson(1),
R. Mauersberger(6,1), A. Linhart(1), L. Bronfman(3),
A.R. Tieftrunk(1,7), K. Meyer(1), W. Wiedenhöver(1),
T.M. Dame(2), E.S. Palmer(2), J. May(3), J. Aparici(3),
F. Mac-Auliffe(3,7)
(1) Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69,
53121 Bonn, Germany
(2) Harvard-Smithsonian Center for Astrophysics, 60 Garden Street,
Cambridge, MA 02138, U.S.A.
(3) Departamento de Astronomía, Universidad de Chile, Casilla 36-D,
Santiago de Chile, Chile
(4) Physics Department, Queen Mary & Westfield College, University of
London, Mile End Road, London E1 4NS, England
(5) Radioastronomisches Institut, Universität Bonn, Auf dem Hügel
71, 53121 Bonn, Germany
(6) Steward Observatory, The University of Arizona, Tucson, AZ 85716,
U.S.A.
(7) Swedish-ESO Submillimetre Telescope, European Southern Observatory,
Casilla 19001, Santiago de Chile 19, Chile
Paper: A&A Supplement Series in press (received 1 July 1996 /
accepted 24 February 1997)
Abstract:
A large scale survey of the Galactic center region in the C18O(J = 1 ->
0) transition is presented. This survey was obtained with the 1.2m
Southern Millimeter-Wave Telescope (SMWT) at the Cerro Tololo
Interamerican Observatory (CTIO) near La Serena, Chile. It covers the
region -1.05 degree <= l <= +3.6 degree and -0.9 degree <= b
<= +0.75 degree with a grid spacing of 9', i.e. the sampling is at
full FWHP beamwidth. 357 positions were in total observed. After
reviewing the instrumentation of the 1.2m SMWT, the observing
techniques, and the methods used in the data reduction, the data of the
survey are presented and morphologically described. In addition, data
of the HNCO(5_0,5-4_0,4) line are presented, which was also included in
the large bandwidth of the spectrometer. 12CO(1-0) measurements
performed for comparison purposes are presented and compared with other
12CO results. The maps of the C18O(1-0) survey demonstrate that there
are great differences between the distribution of the optically thin
C18O(1-0) emission and the usually optically thick 12CO(1-0) emission.
Preprints available from the authors at
G.Dahmen@qmw.ac.uk.
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