2012A&A...540A.119N


Query : 2012A&A...540A.119N

2012A&A...540A.119N - Astronomy and Astrophysics, volume 540A, 119-119 (2012/4-1)

A 3D view of the outflow in the Orion Molecular Cloud 1 (OMC-1).

NISSEN H.D., CUNNINGHAM N.J., GUSTAFSSON M., BALLY J., LEMAIRE J.-L., FAVRE C. and FIELD D.

Abstract (from CDS):

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. 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). 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 2.122µm obtained with the GriF instrument on the Canada-France-Hawaii Telescope, the Apache Point Observatory, the Anglo-Australian Observatory, and the Subaru Telescope. 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 λ720 years ago from a distorted ring-like structure of ∼15'' (6000AU) 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.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: general - methods: numerical - ISM: individual objects: OMC-1

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1148 2
2 V* V2254 Ori Or* 05 35 14.11296 -05 22 22.7316           B 311 2
3 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2251 1
4 COUP 621 Y*O 05 35 14.35371 -05 22 32.8820           ~ 106 0
5 JCMTSE J053514.4-052232 Y*? 05 35 14.488 -05 22 32.10           ~ 48 0
6 [RLK73] IRc 2a Y*O 05 35 14.511 -05 22 30.40           ~ 112 0
7 V* V1330 Ori BY* 05 35 14.9155657944 -05 22 39.203240880   15.040 13.940   11.632 K4 71 0
8 NAME Ori Trapezium OpC 05 35 16.5 -05 23 14           ~ 1598 1
9 M 42 HII 05 35 17 -05 23.4           ~ 4024 0
10 NAME Sgr Arm PoG 19 00 -30.0           ~ 624 1

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2023.09.26-01:11:01

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