Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster

Dzib, Sergio A.; Loinard, Laurent; Rodrı́guez, Luis F.; Gómez, Laura; Forbrich, Jan; Menten, K. M.; Kounkel, Marina; Mioduszewski, Amy J.; Hartmann, L.; Tobin, John J.; Rivera, Juana L.

doi:10.3847/1538-4357/834/2/139

Cited by 51 publications

(74 citation statements)

References 37 publications

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“…This implies that the one-dimensional velocity dispersion in Taurus is somewhat higher than the value of 1km s −1 adopted by Luhman et al (2009) and smaller than the value of 6km s −1 estimated by Bertout & Genova (2006). This value is also similar to the one-dimensional velocity dispersion obtained by Dzib et al (2017) and Kounkel et al (2017) for YSOs in the Orion Nebula Cluster.…”

Section: Taurus (All Stars)supporting

confidence: 75%

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Galli

Loinard

Ortiz-León

et al. 2018

ApJ

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100

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We present new trigonometric parallaxes and proper motions of young stellar objects in the Taurus molecular cloud complex from observations collected with the Very Long Baseline Array as part of the Gould's Belt Distances Survey. We detected 26 young stellar objects and derived trigonometric parallaxes for 18 stars with an accuracy of 0.3% to a few percent. We modeled the orbits of six binaries and determined the dynamical masses of the individual components in four of these systems (V1023 Tau, T Tau S, V807 Tau, and V1000 Tau). Our results are consistent with the first trigonometric parallaxes delivered by the Gaia satellite and reveal the existence of significant depth effects. We find that the central portion of the dark cloud Lynds1495 is located at d= 129.5±0.3 pc, while the B216 clump in the filamentary structure connected to it is at d=158.1±1.2 pc. The closest and remotest stars in our sample are located at d=126.6±1.7 pc and d=162.7±0.8 pc, yielding a distance difference of about 36pc. We also provide a new distance estimate for HLTau that was recently imaged. Finally, we compute the spatial velocity of the stars with published radial velocity and investigate the kinematic properties of the various clouds and gas structures in this region.

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Section: Taurus (All Stars)supporting

confidence: 75%

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Galli

Loinard

Ortiz-León

et al. 2018

ApJ

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100

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“…40 14.39 14.38 14.37 14.36 14.35 14.34 14.33 14.32 40 14.39 14.38 14.37 14.36 14.35 14.34 14.33 14.32 7. THE PROPER MOTIONS OF IRC23 AND ZAPATA 11 Dzib et al (2017) found that the radio sources IRc23 and Zapata 11 also seem to show proper motions receding from the same point from which the other sources are escaping. We use the four new epochs to test this hypothesis and fully confirm the significant large proper motions of these two additional sources.…”

Section: Rotation In the Radio Source?mentioning

confidence: 98%

“…The compact objects that have well measured proper motions are BN, I, n, and more recently source x, studied in the near-infrared by Luhman et al (2017). In addition, Dzib et al (2017) proposed that the sources Zapata 11 and IRc 23 may also be part of the group of receding sources.…”

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confidence: 99%

Proper Motions of the Radio Source Orion MR, Formerly Known as Orion n, and New Sources with Large Proper Motions in Orion BN/KL

Rodrı́guez

Dzib

Zapata

et al. 2020

ApJ

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The infrared source known as Orion n was detected in 1980 with observations made with the 3.8-m United Kingdom Infrared Telescope. About two decades later, sensitive observations made with the Very Large Array revealed the presence of a mJy double radio source apparently coincident in position with the infrared source n. The radio source was assumed to be the counterpart of the infrared source. However, over the years it has been concluded that the radio source shows large proper motions to the south while the infrared source n is stationary. Here we reanalyze the proper motions of the radio source adding both older and newer VLA observations than previously used. We confirm the proper motions of the radio source that at present no longer coincides positionally with the infrared source. The solution to this problem is, most probably, that the infrared source n and the radio source are not the same object: the infrared source is a stationary object in the region while the radio counterpart is moving as a result of the explosion that took place in this region some 500 years ago and that expelled large amounts of molecular gas as well as several compact sources. Considering the paper where it was first reported, we refer to this double radio source as Orion MR.In addition, we use these new observations to fully confirm the large proper motions of the sources IRc23 and Zapata 11. Together with sources BN, I, Orion MR, and x, there are at least six compact sources that recede from a point in common in Orion BN/KL. However, IRc23 is peculiar in that its ejection age appears to be only ∼300 years. The relatively large number of sources rules out as a possible mechanism the classic three-body scenario since then only two escaping bodies are expected: a tight binary plus the third star involved in the encounter.

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“…We estimated the errors in these motions from the standard deviations of the differences in right ascension and declination between the two epochs. These estimates are upper limits for the errors since the velocity dispersion among the stars (∼ 1 mas yr −1 , van Altena et al 1988;Dzib et al 2017) also contributes to the dispersion in our proper motion measurements.…”

Section: Astrometry In the Kleinmann-low Nebulamentioning

confidence: 99%

“…For one of these massive stars, the Becklin-Neugebauer (BN) object (Becklin & Neugebauer 1967), multi-epoch radio observations have revealed an unusually high proper motion (Plambeck et al 1995). Members of Orion exhibit a dispersion of ∼ 1 mas yr −1 in their proper motions (van Altena et al 1988;Dzib et al 2017), whereas BN has a proper motion of 13.5 mas yr −1 (26 km s −1 ) relative to the cluster .…”

Section: Introductionmentioning

confidence: 99%

New Evidence for the Dynamical Decay of a Multiple System in the Orion Kleinmann–Low Nebula*

Luhman

Robberto

Tan

et al. 2017

ApJL

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We have measured astrometry for members of the Orion Nebula Cluster with images obtained in 2015 with the Wide Field Camera 3 on board the Hubble Space Telescope. By comparing those data to previous measurements with NICMOS on Hubble in 1998, we have discovered that a star in the Kleinmann-Low Nebula, source x from Lonsdale et al. (1982), is moving with an unusually high proper motion of 29 mas yr −1 , which corresponds to 55 km s −1 at the distance of Orion. Previous radio observations have found that three other stars in the Kleinmann-Low Nebula (BN and sources I and n) have high proper motions (5-14 mas yr −1 ) and were near a single location ∼540 years ago, and thus may have been members of a multiple system that dynamically decayed. The proper motion of source x is consistent with ejection from that same location 540 years ago, which provides strong evidence that the dynamical decay did occur and that the runaway star BN originated in the Kleinmann-Low Nebula rather than the nearby Trapezium cluster. However, our constraint on the motion of source n is significantly smaller than the most recent radio measurement, which indicates that it did not participate in the event that ejected the other three stars.

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Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster

Cited by 51 publications

References 37 publications

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Proper Motions of the Radio Source Orion MR, Formerly Known as Orion n, and New Sources with Large Proper Motions in Orion BN/KL

New Evidence for the Dynamical Decay of a Multiple System in the Orion Kleinmann–Low Nebula*

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