Volume 540, April 2012
|Number of page(s)||11|
|Section||Interstellar and circumstellar matter|
|Published online||09 April 2012|
1 Department of Physics and Astronomy, University of Århus, Ny Munkegade, 8000 Århus C, Denmark
e-mail: firstname.lastname@example.org; email@example.com, firstname.lastname@example.org
2 Department of Physics and Astronomy, University of Nebraska-Lincoln 116 Brace Laboratory, Lincoln, NE 68588-0111, USA
3 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
4 Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA
5 LAMAp/LERMA, UMR8112 du CNRS, de l’Observatoire de Paris et de l’Université de Cergy Pontoise, 95031 Cergy Pontoise Cedex, France
Received: 16 June 2011
Accepted: 9 March 2012
Context. Stars whose mass is an order of magnitude greater than the Sun play a prominent role in the evolution of galaxies, exploding as supernovae, triggering bursts of star formation and spreading heavy elements about their host galaxies. A fundamental aspect of star formation is the creation of an outflow. The fast outflow emerging from a region associated with massive star formation in the Orion Molecular Cloud 1 (OMC-1), located behind the Orion Nebula, appears to have been set in motion by an explosive event.
Aims. We study the structure and dynamics of outflows in OMC-1. We combine radial velocity and proper motion data for near-IR emission of molecular hydrogen to obtain the first 3-dimensional (3D) structure of the OMC-1 outflow. Our work illustrates a new diagnostic tool for studies of star formation that will be exploited in the near future with the advent of high spatial resolution spectro-imaging in particular with data from the Atacama Large Millimeter Array (ALMA).
Methods. We used published radial and proper motion velocities obtained from the shock-excited vibrational emission in the H2 v = 1−0 S(1) line at 2.122 μm obtained with the GriF instrument on the Canada-France-Hawaii Telescope, the Apache Point Observatory, the Anglo-Australian Observatory, and the Subaru Telescope.
Results. These data give the 3D velocity of ejecta yielding a 3D reconstruction of the outflows. This allows one to view the material from different vantage points in space giving considerable insight into the geometry. Our analysis indicates that the ejection occurred ≲720 years ago from a distorted ring-like structure of ~15″ (6000 AU) in diameter centered on the proposed point of close encounter of the stars BN, source I and maybe also source n. We propose a simple model involving curvature of shock trajectories in magnetic fields through which the origin of the explosion and the center defined by extrapolated proper motions of BN, I and n may be brought into spatial coincidence.
Key words: stars: formation / stars: general / methods: numerical / ISM: individual objects: OMC-1
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.
© ESO, 2012
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