The distance to the Orion Nebula

Abstract

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.

13 pages, 3 figures, to appear in Astronomy & Astrophyiscs

References in corpus (1)

• Imaging the Ionized Disk of the High-Mass Protostar Orion-I

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• Properties of the ionized gas in HH202. II: Results from echelle spectrophotometry with UVES
• Proplyds and Massive Disks in the Orion Nebula Cluster Imaged with CARMA and SMA
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• A Multi-Color Optical Survey of the Orion Nebula Cluster. Part I: the Catalog
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• The Circumstellar Disk Mass Distribution in the Orion Trapezium Cluster
• High-Resolution Chandra X-ray Imaging and Spectroscopy of the Sigma Orionis Cluster
• High Velocity Features in the Orion Nebula
• A 1.3 cm wavelength radio flare from a deeply embedded source in the Orion BN/KL region
• Tidal foces as a regulator of star formation in Taurus
• Encounters in the ONC - observing imprints of star-disc interactions
• High Resolution Radio Astronomy Using Very Long Baseline Interferometry
• Optical interferometric observations of Theta 1 Orionis C from NPOI and implications for the system orbit
• High Angular Resolution Observations at 7-mm of the Core of the Quadrupolar HH 111/121 Outflow
• Evidence for a Photoevaporated Circumbinary Disk in Orion
• Infall and rotation motions in the HH 111 protostellar system: A flattened envelope in transition to a disk?