VLBA Determination of the Distance to Nearby Star-forming Regions. VIII. The LkHα 101 Cluster

Dzib, Sergio A.; Ortiz-León, Gisela N.; Loinard, Laurent; Mioduszewski, Amy J.; Rodrı́guez, Luis F.; Medina, S.; Torres, Rosa M.

doi:10.3847/1538-4357/aaa431

Cited by 10 publications

(6 citation statements)

References 20 publications

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“…Despite its large size and mass, the CMC appears to be very modest in its star formation activity. In the CMC, the LkHα 101 embedded cluster is the first and only one significant cluster, which is also consistent with the LkHα 101 H II region (Barsony et al 1990;Dzib et al 2018). In the embedded cluster, the star LkHα 101 is a young high-mass star with a spectral type of near B0.5 (Herbig et al 2004;Wolk et al 2010).…”

Section: Introductionsupporting

confidence: 76%

“…In the CMC or main filament, the LkHα 101 embedded cluster with an H II region and several B0.5 stars is the first and only one significant cluster (Barsony et al 1990;Dzib et al 2018). We see that the LkHα 101 embedded cluster is just located at the projected intersectional position of the main filamnet with the minor filament.…”

Section: The Lkh 101 Embedded Cluster Formationmentioning

confidence: 73%

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First Embedded Cluster Formation in California Molecular Cloud

Jiang

et al. 2020

ApJL

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We performed a multi-wavelength observation toward LkHα 101 embedded cluster and its adjacent 85 × 60 region. The LkHα 101 embedded cluster is the first and only one significant cluster in California molecular cloud (CMC). These observations have revealed that the LkHα 101 embedded cluster is just located at the projected intersectional region of two filaments. One filament is the highest-density section of the CMC, the other is a new identified filament with a low-density gas emission. Toward the projected intersection, we find the bridging features connecting the two filaments in velocity, and identify a V-shape gas structure. These agree with the scenario that the two filaments are colliding with each other. Using the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we measured that the RRL velocity of the LkH 101 H II region is 0.5 km s −1 , which is related to the velocity component of the CMC filament. Moreover, there are some YSOs distributed outside the intersectional region. We suggest that the cloud-cloud collision together with the fragmentation of the main filament may play an important role in the YSOs formation of the cluster.

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Section: Introductionsupporting

confidence: 76%

Section: The Lkh 101 Embedded Cluster Formationmentioning

confidence: 73%

First Embedded Cluster Formation in California Molecular Cloud

Jiang

et al. 2020

ApJL

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“…Previously, parallax and PMs have been measured for a number of young stars with the Very Long Baseline Array (Melis et al 2014;Ortiz-León et al 2017a;Kounkel et al 2017c;Ortiz-León et al 2017b;Dzib et al 2018;Galli et al 2018). The precision of these observations is comparable to that of Gaia DR2.…”

Section: Gaiamentioning

confidence: 99%

The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure

Kounkel¹,

Covey²,

Suárez³

et al. 2018

318

455

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We present an analysis of spectrosopic and astrometric data from APOGEE-2 and Gaia DR2 to identify structures towards the Orion Complex. By applying a hierarchical clustering algorithm to the 6-dimensional stellar data, we identify spatially and/or kinematically distinct groups of young stellar objects with ages ranging from 1 to 12 Myr. We also investigate the star forming history within the Orion Complex, and identify peculiar sub-clusters. With this method we reconstruct the older populations in the regions that are presently largely devoid of molecular gas, such as Orion C (which includes the σ Ori cluster), and Orion D (the population that traces Ori OB1a, OB1b, and Orion X). We report on the distances, kinematics, and ages of the groups within the Complex. The Orion D groups is in the process of expanding. On the other hand, Orion B is still in the process of contraction. In λ Ori the proper motions are consistent with a radial expansion due to an explosion from a supernova; the traceback age from the expansion exceeds the age of the youngest stars formed near the outer edges of the region, and their formation would have been triggered when they were half-way from the cluster center to their current positions. We also present a comparison between the parallax and proper motion solutions obtained by Gaia DR2, and those obtained towards star-forming regions by Very Long Baseline Array.

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“…see next subsection). In recent years, Very Long Baseline Interferometry (VLBI) has helped to estimate the distance with a few percents of accuracy to Young Stellar Objects (YSOs) with strong magnetic activity that produces non-thermal radio emission (e.g., Ortiz-León et al 2017a,b;Kounkel et al 2017;Dzib et al 2018;Galli et al 2018, and references therein). In all cases, these estimations allowed to obtain a mean distance, the depth, and the kinematics of the regions where they belong.…”

Section: Introductionmentioning

confidence: 99%

Distances and Kinematics of Gould Belt Star-forming Regions with Gaia DR2 Results

Dzib

Loinard

Ortiz-León

et al. 2018

ApJ

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119

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We present an analysis of the astrometric results from Gaia second data release (DR2) to Young Stellar Objects (YSOs) in starforming regions related to the Gould Belt. These regions are Barnard 59, Lupus 1 to 4, Chamaeleon I and II, -Chamaeleontis, the Cepheus flare, IC 5146 and Corona Australis. The mean distance to the YSOs in each region are consistent with earlier estimations, though a significant improvement to the final errors was obtained. The mean distances to the star-forming regions were used to fit an ellipsoid of size (358 ± 7) × (316 ± 13) × (70 ± 4) pc, and centered at (X 0 ,Y 0 , Z 0 ) = (−82 ± 15, 39 ± 7, −25 ± 4) pc, consistent with recently determined parameter of the Gould Belt. The mean proper motions were combined with radial velocities from the literature to obtain the three dimensional motion of the star-forming regions, which are consistent with a general expansion of the Gould Belt. We estimate that this expansion is occurring at a velocity of 2.5 ± 0.1 km s −1 . This is the first time that YSOs motions are used to investigate the kinematic of the Gould Belt. As an interesting side result, we also identified stars with large peculiar velocities.

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VLBA Determination of the Distance to Nearby Star-forming Regions. VIII. The LkHα 101 Cluster

Cited by 10 publications

References 20 publications

First Embedded Cluster Formation in California Molecular Cloud

First Embedded Cluster Formation in California Molecular Cloud

The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure

Distances and Kinematics of Gould Belt Star-forming Regions with Gaia DR2 Results

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