The distance to the Orion Nebula

By K. Menten, M. J. Reid, J. Forbrich, A. Brunthaler. 2007

602 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9a4220c9acc5b1e1d9f1f3140b091138cfdbd953

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In Astronomy and Astrophysics

Citations in the corpus

Herschel-Planck dust optical-depth and column-density maps - I. Method description and results for Orion (2014, positive): “It contains the nearest massive star-forming cluster to Earth, the Trapezium cluster (e.g. Hillenbrand 1997; Lada et al. 2000; Muench et al. 2002; Da Rio et al. 2012), at a distance of 414 pc Menten et al. 2007).”
Dynamical mass of the O-type supergiant in ζ Orionis A (2013, background): “The Orion star forming regions are typically assumed to be at about 400 pc. Menten et al. (2007) derived a distance of 414±7 pc from VLBA astrometry to the Orion nebula cluster, confirmed by Kraus et al. (2009), who obtained an orbital parallax from one of its members.”
An ALMA study of the Orion Integral Filament: I. Evidence for narrow fibers in a massive cloud (2018, background): “The resulting ALMA mosaic covers an approximate area of 2.5 × 0.48 pc2 with an effective resolution of 0.009 pc (i.e., θFWHM = 4.5′′ at the distance of 414 pc; Menten et al. 2007).”
Kinematics in Young Star Clusters and Associations with Gaia DR2 (2018, methodology): “• Our analysis of the Gaia data places the ONC at a distance of 403+7−6 pc, which is slightly closer than the estimate of 414±7 pc from Menten et al. (2007), but farther than 388±5 pc found by Kounkel et al. (2017), both based on Very Long Baseline Array (VLBA) data.”
Physical Processes in the Interstellar Medium (2014, background): “It lies at a distance of 410pc (Sandstrom et al., 2007; Menten et al., 2007; Hirota et al., 2007; Caballero, 2008).”
The relation between the most-massive star and its parental star cluster mass (2009, neutral): “…Hasan et al. (2008), 38: Koenig et al. (2008), 39: Turner (1985); Pandey et al. (1989), 40: Hillenbrand & Hartmann (1998); Hillenbrand et al. (1998); Menten et al. (2007); Kraus et al. (2009), 41: Wolk et al. (2006, 2008), 42: Dambis (1999); Lata et al. (2002), 43: Blanco & Williams (1959);…”
THE HIGH ANGULAR RESOLUTION MULTIPLICITY OF MASSIVE STARS (2008, background): “The preliminary orbit indicates a total mass of 32 M for a distance of 414 pc (Menten et al. 2007).”
THE WISE CATALOG OF GALACTIC H ii REGIONS (2013, neutral): “…Hirota et al. 2008c; (13) Honma et al. 2007; (14) Honma et al. 2011; (15) Immer et al. 2013; (16) Jones & Dickey 2012; (17) Kurayama et al. 2011; (18) Menten et al. 2007; (19) Moellenbrock et al. 2009; (20) Moscadelli et al. 2009; (21) Niinuma et al. 2011; (22) Oh et al. 2010; (23) Reid et al.…”
VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. III. HP TAU/G2 AND THE THREE-DIMENSIONAL STRUCTURE OF TAURUS (2009, methodology): “Introduction Several recent observations (e.g. Loinard et al. 2005, 2007, 2008; Torres et al. 2007; Menten et al. 2007; Xu et al. 2006) have demonstrated that multi-epoch VLBI observations can be used to measure the trigonometric parallax of nearby young starsto better than a few percent.”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “This severe underestimate for Orion itself from Hα emission results because the Orion cluster is too small to fully populate the IMF; its earliest spectral type is O7 V, and so the star cluster produces relatively little ionizing luminosity relative to its total mass and SFR.”
SiO Maser Observations toward Orion-KL with VERA (2008, methodology): “However, our present result, 418˙6 pc for Orion-KL, is very consistent with another VLBA result by Menten et al. (2007) with a higher quoted accuracy, 414˙7pc.”
TRIGONOMETRIC PARALLAXES OF HIGH MASS STAR FORMING REGIONS: THE STRUCTURE AND KINEMATICS OF THE MILKY WAY (2014, neutral): “…et al. (2011), 39:Niinuma et al. (2011), 40:Reid et al. (2009a), 41:Shiozaki et al. (2011), 42:Honma et al. (2007), 43:Sandstrom et al. (2007),4 4:Menten et al. (2007), 45:Kim et al. (2008), 46:Choi et al. (2008), 47:Zhang et al. (2012a). most straightforwardly, looking at a plan view of the…”
ON THE NATURE OF THE LOCAL SPIRAL ARM OF THE MILKY WAY (2013, background): “…from its methanol masers (Moscadelli, private communicaiton). dThe parallax of Orion is an unweighted average value of the independent results from Menten et al. (2007) and Kim et al. (2008) with equal accuracy, while the proper motions come fromMenten et al. (2007), because Hirota et al. (2007)…”
THE HERSCHEL ORION PROTOSTAR SURVEY: SPECTRAL ENERGY DISTRIBUTIONS AND FITS USING A GRID OF PROTOSTELLAR MODELS (2016, background): “This is the largest sample of protostars studied in a single, nearby starforming region (distance of 420 pc; Menten et al. 2007; Kim et al. 2008) and therefore significant for advancing our understanding of protostellar structure and evolution.”
Microarcsecond Radio Astrometry (2013, methodology): “Recently, two very accurate parallaxes have been published: Menten et al. (2007) used the VLBA and observed continuum emission from three YSOs and determined a distance of 414±7 pc; Kim et al. (2008) using VERA and observing SiO masers estimated a distance of 418±6 pc.”
Parallaxes and proper motions of interstellar masers toward the Cygnus X star-forming complex. I. Membership of the Cygnus X region (2011, background): “…Arm: green dots mark sources from this work; red dots mark sources from the literature (from left to right): Choi et al. (2008), Reid et al. (2009a), Hirota et al. (2007); Menten et al. (2007), Hirota et al. (2008a), Hirota et l. (2011), Moscadelli et al. (2009), Rygl et al. (2010), Hirotae al.”