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Title:
Observations of spatial and velocity structure in the Orion molecular cloud
Authors:
Nissen, H. D.; Gustafsson, M.; Lemaire, J. L.; Clénet, Y.; Rouan, D.; Field, D.
Affiliation:
AA(Department of Physics and Astronomy, University of Aarhus, 8000 Aarhus C, Denmark ), AB(Department of Physics and Astronomy, University of Aarhus, 8000 Aarhus C, Denmark), AC(Observatoire de Paris and Université de Cergy-Pontoise, LERMA and UMR 8112 du CNRS, 92195 Meudon, France), AD(Observatoire de Paris-Meudon, LESIA, 92195 Meudon Principal Cedex, France), AE(Observatoire de Paris-Meudon, LESIA, 92195 Meudon Principal Cedex, France), AF(Department of Physics and Astronomy, University of Aarhus, 8000 Aarhus C, Denmark)
Publication:
Astronomy and Astrophysics, Volume 466, Issue 3, May II 2007, pp.949-968 (A&A Homepage)
Publication Date:
05/2007
Origin:
EDP Sciences
Keywords:
ISM: jets and outflows, ISM: structure, stars: formation, stars: circumstellar matter, ISM: kinematics and dynamics, ISM: molecules
DOI:
10.1051/0004-6361:20054304
Bibliographic Code:
2007A&A...466..949N

Abstract

Observations are reported of H2 IR emission in the S(1) v=1-0 line at 2.121 μm in the Orion Molecular Cloud, OMC1, using the GriF instrument on the Canada-France-Hawaii Telescope. GriF uses a combination of adaptive optics and Fabry-Perot interferometry, yielding a spatial resolution of 0.15´´ to 0.18´´ and velocity discrimination as high as 1 km s-1. 193 bright H2 emission regions can be identified in OMC1. The general characteristics of these features are described in terms of radial velocities, brightness and spatial displacement of maxima of velocity and brightness, the latter to yield the orientation of flows in the plane of the sky. Strong spatial correlation between velocity and bright H2 emission is found and serves to identify many features as shocks. Important results are: (i) velocities of the excited gas illustrate the presence of a zone to the south of BN-IRc2 and Peak 1, and the west of Peak 2, where there is a powerful blue-shifted outflow with an average velocity of -18 km s-1. This is shown to be the NIR counterpart of an outflow previously identified in the radio, originating from either source I or source n. (ii) There is a band of weak radial velocity features (<5 km s-1) in Peak 1. (iii) A small proportion of the flows may represent sites of low mass star formation and one region shows evidence of multiple flows which may indicate multiple low mass star formation within OMC1.

Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Tables A.1-A.3 are only available in electronic form at http://www.aanda.org

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