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The distance to the Orion Nebula
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We have used the Very Long Baseline Array to measure the trigonometric parallax of several member stars of the Orion Nebula Cluster showing non-thermal radio emission. We have determined the distance to the cluster to be 414 +/- 7 pc. Our distance determination allows for an improved calibration of luminosities and ages of young stars. We have also measured the proper motions of four cluster stars which, when accurate radial velocities are measured, will put strong constraints on the origin of the cluster.
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Cited by 5 Pith papers
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Resolving dense photo-dissociation regions: the structure of photochemical fronts in three-dimensional gas distributions
A three-dimensional PDR model shows that overlapping H2 dissociation and C+ recombination fronts, plus the arc-like H2 emission seen in the Orion Bar, arise from shadowing by dense clumps in a fractal gas distribution.
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Dust Seeding Molecules in a Massive Protostar -- Detection of TiO in Orion Source I
TiO is detected for the first time in a star-forming region, traced to the base of the rotating outflow of Orion Source I with a column density implying efficient dust-to-gas conversion.
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PDRs4All XXII. Near-Infrared continuum in the Orion Bar
The near-infrared excess in the Orion Bar decomposes into a ~700 K component correlated with the 3.3 micrometer aromatic band and a weakly constrained hotter component that is not.
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Emergence of high-mass stars in complex fiber networks (EMERGE) VI. Turbulence dissipation and the formation of dense fibers
In Orion, turbulence dissipates in high-shear regions near dense fibers, so the transition to coherence occurs at the fiber level before cores form.
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Scattered light signatures of flyby-induced warps in protoplanetary discs
Flyby-induced warps create observable oscillating shadows in scattered light for low-viscosity discs lasting most of their ~10^6 year lifetime, enabling surveys to probe viscosity.
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