EDP Sciences
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Volume 402, Number 3, May II 2003
First Science with the ODIN satellite
Page(s) L39 - L46
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20030337

A&A 402, L39-L46 (2003)
DOI: 10.1051/0004-6361:20030337


Highlights from the first year of Odin observations

Å. Hjalmarson1, U. Frisk2, M. Olberg1, P. Bergman1, P. Bernath3, N. Biver4, 5, J. H. Black1, R. S. Booth1, V. Buat6, J. Crovisier5, C. L. Curry3, M. Dahlgren1, P. J. Encrenaz7, E. Falgarone8, P. A. Feldman9, M. Fich3, H. G. Florén10, M. Fredrixon1, M. Gerin8, E. M. Gregersen11, M. Hagström1, J. Harju12, T. Hasegawa13, C. Horellou1, L. E. B. Johansson1, E. Kyrölä14, S. Kwok13, B. Larsson10, A. Lecacheux5, T. Liljeström15, M. Lindqvist1, R. Liseau10, E. J. Llewellyn16, K. Mattila12, G. Mégie17, G. F. Mitchell18, D. Murtagh19, L.-Å. Nyman20, H. L. Nordh21, A. O. H. Olofsson1, G. Olofsson10, H. Olofsson10, L. Pagani7, G. Persson1, R. Plume13, H. Rickman22, I. Ristorcelli23, G. Rydbeck1, Aa. Sandqvist10, F. von Schéele2, G. Serra23, S. Torchinsky24, N. F. Tothill18, K. Volk13, T. Wiklind1, C. D. Wilson11, A. Winnberg1 and G. Witt25

1  Onsala Space Observatory, 439 92 Onsala, Sweden
2  Swedish Space Corporation, PO Box 4207, 171 04 Solna, Sweden
3  Department of Physics, University of Waterloo, Waterloo, ON N2L 3G1, Canada
4  ESA-ESTEC, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands
5  LESIA & FRE 2461 de CNRS, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon Cedex, France
6  Laboratoire d'Astronomie Spatiale, BP 8, 13376 Marseille Cedex 12, France
7  LERMA & FRE 2460 du CNRS, Observatoire de Paris, 61 Av. de l'Observatoire, 75140 Paris, France
8  LERMA & FRE 2460 du CNRS, École Normale Supérieure, 24 rue Lhomond, 75005 Paris, France
9  NRC Canada, Herzberg Inst. of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
10  Stockholm Observatory, SCFAB, Roslagstullsbacken 21, 106 91 Stockholm, Sweden
11  Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada
12  Observatory, PO Box 14, University of Helsinki, 00014 Helsinki, Finland
13  Department of Physics and Astronomy, University of Calgary, Calgary, ABT 2N 1N4, Canada
14  Finnish Meteorological Institute, PO Box 503, 00101 Helsinki, Finland
15  Metsähovi Radio Observatory, Helsinki University of Technology, Otakaari 5A, 02150 Espoo, Finland
16  Department of Physics and Engineering Physics, 116 Science Place, University of Saskatchewan, Saskatoon, SK S7N 5E2, Canada
17  Institut Pierre Simon Laplace, CNRS-Université Paris 6, 4 place Jussieu, 75252 Paris Cedex 05, France
18  Department of Astronomy and Physics, Saint Mary's University, Halifax, NS B3H 3C3, Canada
19  Global Environmental Measurements Group, Chalmers University of Technology, 412 96 Göteborg, Sweden
20  ESO, Casilla 19001, Santiago 19, Chile
21  Swedish National Space Board, PO Box 4006, 171 04 Solna, Sweden
22  Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden
23  CESR, 9 Avenue du Colonel Roche, BP 4346, 31029 Toulouse, France
24  Canadian Space Agency, St-Hubert, J3Y 8Y9, Québec, Canada
25  Department of Meteorology, Stockholm University, 106 91 Stockholm, Sweden

(Received 3 December 2002 / Accepted 28 January 2003)

Key Odin operational and instrumental features and highlights from our sub-millimetre and millimetre wave observations of H 2O, H 218O, NH 3, 15NH 3 and O 2 are presented, with some insights into accompanying Odin Letters in this A&A issue. We focus on new results where Odin's high angular resolution, high frequency resolution, large spectrometer bandwidths, high sensitivity or/and frequency tuning capability are crucial: H 2O mapping of the Orion KL, W 3, DR 21, S 140 regions, and four comets; H 2O observations of Galactic Centre sources, of shock enhanced H 2O towards the SNR IC 443, and of the candidate infall source IRAS 16293-2422; H 218O detections in Orion KL and in comet Ikeya-Zhang; sub-mm detections of NH 3 in Orion KL (outflow, ambient cloud and bar) and $\rho$ Oph, and very recently, of  15NH 3 in Orion KL. Simultaneous sensitive searches for the 119 GHz line of O 2 have resulted in very low abundance limits, which are difficult to accomodate in chemical models. We also demonstrate, by means of a quantitative comparison of Orion KL H 2O results, that the Odin and SWAS observational data sets are very consistently calibrated.

Key words: radio lines: ISM -- ISM: molecules -- space vehicles: instruments -- submillimeter -- techniques: spectroscopic -- telescopes

Offprint request: Å. Hjalmarson, hjalmar@oso.chalmers.se

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