New Expansion Rate Estimate of the Scorpius–Centaurus Association Based on T Tauri Stars from the Gaia DR2 Catalog

Бобылев, В. В.; Baykova, A. T.

doi:10.1134/s1063772920040022

Cited by 7 publications

(2 citation statements)

References 35 publications

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“…An analysis using Gaia DR1 data (Gaia Collaboration et al 2016b, ∼400 stars) by Wright & Mamajek (2018) found no evidence that the three Sco-Cen subgroups were more compact in the past, but did confirm that the stars are gravitationally unbound and have a nonisotropic velocity dispersion. On the other hand, Bobylev & Baykova (2020) estimate a linear expansion coefficient of Sco-Cen to be 39 ± 2 km s −1 kpc −1 , based on T Tauri stars.…”

Section: Introductionmentioning

confidence: 97%

Chronostar. II. Kinematic age and substructure of the Scorpius-Centaurus OB2 association

Žerjal,

Ireland,

Crundall

et al. 2021

Preprint

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The nearest region of massive star formation -the Scorpius-Centaurus OB2 association (Sco-Cen) -is a local laboratory ideally suited to the study of a wide range of astrophysical phenomena. Precision astrometry from the Gaia mission has expanded the census of this region by an order of magnitude. However, Sco-Cen's vastness and complex substructure make kinematic analysis of its traditional three regions, Upper Scorpius, Upper Centaurus-Lupus and Lower Centaurus-Crux, challenging. Here we use C , a Bayesian tool for kinematic age determination, to carry out a new kinematic decomposition of Sco-Cen using full 6-dimensional kinematic data. Our model identifies 8 kinematically distinct components consisting of 8,185 stars distributed in dense and diffuse groups, each with an independentlyfit kinematic age; we verify that these kinematic estimates are consistent with isochronal ages. Both Upper Centaurus-Lupus and Lower Centaurus-Crux are split into two parts. The kinematic age of the component that includes PDS 70, one of the most well studied systems currently forming planets, is 15±3 Myr.

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Section: Introductionmentioning

confidence: 97%

Chronostar. II. Kinematic age and substructure of the Scorpius-Centaurus OB2 association

Žerjal,

Ireland,

Crundall

et al. 2021

Preprint

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“…There are several small associations and compact moving groups of very young (5)(6)(7)(8)(9)(10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20) stars near the Sun. This is, for example, Tucana, β Pic, η Cha, ϵ Cha, TW Hya.…”

Section: Introductionmentioning

confidence: 99%

Study of the structure and kinematics of the Galaxy according to VLBI-astrometry of masers and radio stars

Bobylev¹,

Bajkova²

2022

Publ. Pulk. Obs.

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In recent years, radio interferometric observations have achieved high accuracy in determining the absolute values of trigonometric parallaxes and proper motions of maser radiation sources and radio stars. The error in determining the trigonometric parallaxes of these objects averages about 10 microarcseconds, which allows us to confidently study the geometric and kinematic properties of the distribution of stars located at great distances from the Sun, up to the center of the Galaxy. This article provides an overview of the main results of studying the structure and kinematics of the Galaxy, which were obtained by various scientific teams using VLBI observations of masers and radio stars. The main attention is paid to the results of studying the Galaxy obtained by the authors of this work.

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OB Associations and their origins

Wright

2020

New Astronomy Reviews

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OB associations are unbound groups of young stars made prominent by their bright OB members, and have long been thought to be the expanded remnants of dense star clusters. They have been important in astrophysics for over a century thanks to their luminous massive stars, though their low-mass members have not been well studied until the last couple of decades. This has changed thanks to data from X-ray observations, spectroscopic surveys and astrometry from Gaia that allows their full stellar content to be identified and their dynamics to be studied, which in turn is leading to changes in our understanding of these systems and their origins, with the old picture of Blaauw (1964a) now being superseded. It is clear now that OB associations have considerably more substructure than once envisioned, both spatially, kinematically and temporally. These changes have implications for the star formation process, the formation and evolution of planetary systems, and the build-up of stellar populations across galaxies.

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New Expansion Rate Estimate of the Scorpius–Centaurus Association Based on T Tauri Stars from the Gaia DR2 Catalog

Cited by 7 publications

References 35 publications

Chronostar. II. Kinematic age and substructure of the Scorpius-Centaurus OB2 association

Chronostar. II. Kinematic age and substructure of the Scorpius-Centaurus OB2 association

Study of the structure and kinematics of the Galaxy according to VLBI-astrometry of masers and radio stars

OB Associations and their origins

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