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Astron. Astrophys. 322, L33-L36 (1997)
Letter to the Editor
Detection of [O I] 63 ![[FORMULA]](img1.gif)
m in absorption toward Sgr B2
*
J.-P. Baluteau 1,
P. Cox 2,
J. Cernicharo 3,
D. Péquignot 4,
E. Caux 5,
T. Lim 6,
B. Swinyard 7,
G. White 8,
M. Kessler 9,
T. Prusti 9,
M. Barlow 10,
P.E. Clegg 8,
R.J. Emery 7,
I. Furniss 10,
W. Glencross 10,
C. Gry 1, 6,
M. Joubert 1,
R. Liseau 11,
B. Nisini 11,
P. Saraceno 11,
G. Serra 5,
C. Armand 6,
M. Burgdorf 6,
A. DiGiorgio 6,
S. Molinari 6,
M. Price 6,
D. Texier 6,
S. Sidher 6 and
N. Trams 6
1 Laboratoire d'Astronomie Spatiale, LP CNRS, BP 8,
F-13376 Marseille Cedex 12, France
2 Institut d'Astrophysique Spatiale, Bât. 120,
Université Paris XI, F-91405 Orsay Cedex, France
3 CSIC. IEM. Dpto. Fisica Molecular, Serrano 123, E-28006
Madrid, Spain & OAN, Ap 1143, E-28800 A. de Henares, Spain
4 DAEC, Observatoire de Paris-Meudon, F-92195 Meudon Cedex,
France
5 Centre d'Etude Spatiale des Rayonnements, CESR/CNRS-UPS,
BP 4346, F-31028 Toulouse Cedex 04, France
6 The LWS Instrument Dedicated Team, ISO Science Operations
Centre, PO Box 50727, E-28080 Madrid, Spain
7 Rutherford Appleton Lab., Chilton, Didcot, Oxon OX11 0QX,
UK
8 Queen Mary and Westfield College, University of London,
Mile End Road, London E1 4NS, UK
9 ISO Science Operations Centre, Astrophysics Division of
ESA, PO Box 50727, E-28080 Madrid, Spain
10 Department of Physics and Astronomy, University College
London, Gower Street, London WC1E 6BT, UK
11 CNR-Instituto di Fisica dello Spazio Interplanetario,
Casella Postale 27, I-00044 Frascati, Italy
Received 17 December 1996 / Accepted 9 January 1997
Abstract
A high signal-to-noise 52-90 µm spectrum is presented
for the central part of the Sagittarius B2 complex. The data were
obtained with the Long Wavelength Spectrometer on board the Infrared
Space Observatory (ISO). The [O I] 63 µm line
is detected in absorption even at the grating spectral resolution of
0.29 µm. A lower limit for the column density of
atomic oxygen of the order of ![[FORMULA]](img2.gif)
cm-2 is
derived. This implies that more than 40% of the interstellar oxygen
must be in atomic form along the line of sight toward the Sgr B2
molecular cloud.
Key words: ISM:
abundances 
(ISM:) dust,
extinction
(ISM:) H II
regions
ISM: individual objects:
Sgr B2
Infrared: ISM:
continuum
Infrared: ISM: lines and bands
* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA
Send offprint requests to: J.-P. Baluteau (baluteau@astrsp-mrs.fr)
Contents
© European Southern Observatory (ESO) 1997
Online publication: June 5, 1998
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