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Issue A&A
Volume 411, Number 3, December I 2003
Page(s) 437 - 446
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20031013



A&A 411, 437-446 (2003)
DOI: 10.1051/0004-6361:20031013

New insight into shocks and star formation in Orion: First light with GriF

M. Gustafsson1, L. E. Kristensen1, Y. Clénet2, D. Field1, J. L. Lemaire3, 4, G. Pineau des Forêts5, D. Rouan2 and E. Le Coarer6

1  Department of Physics and Astronomy, University of Aarhus, 8000 Aarhus C, Denmark
2  Observatoire de Paris-Meudon, LESIA, 92195 Meudon Principal Cedex, France
3  Observatoire de Paris-Meudon, LERMA and UMR8112 of the CNRS, 92195 Meudon Principal Cedex, France
4  Université de Cergy-Pontoise, LERMA and UMR8112 of the CNRS, 95806 Cergy Cedex, France
5  Institut d'Astrophysique Spatiale, Université Paris XI, 91405 Orsay Cedex, France
6  Observatoire de Grenoble, Laboratoire d'Astrophysique de l'Observatoire de Grenoble, France

(Received 20 January 2003 / Accepted 30 June 2003)

Abstract
A new instrument, "GriF", has been used on the Canada-France-Hawaii Telescope to record spatially and velocity resolved images, in the H 2 v=1-0 S(1) line in the K-band, of a $1'\times1'$ field in the core of the Orion Molecular Cloud, OMC1. Using the PUEO adaptive optics system combined with Fabry-Perot interferometry, diffraction limited spatial resolution of 0 $\farcs$15 and velocity discrimination of ~1 kms -1 has been achieved. These data yield graphic images of shocks in OMC1, presenting a level of detail which has not previously been attained. Observed structures suggest that a significant fraction of the regions strongly emitting in H 2 do so through local, internal shocks, associated with star formation within the clumps of gas involved. Thus the core of OMC1 is revealed for the first time as a region which contains a number of developed protostars.


Key words: ISM: individual objects: OMC1 -- ISM: kinematics and dynamics -- ISM: molecules -- shock waves -- ISM: lines and bands -- stars: formation

Offprint request: D. Field, dfield@phys.au.dk

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© ESO 2003


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