Kinematics in Young Star Clusters and Associations withGaiaDR2

  title={Kinematics in Young Star Clusters and Associations withGaiaDR2},
  author={Michael A. Kuhn and L. A. Hillenbrand and Alison Sills and Eric D. Feigelson and Konstantin V. Getman},
  journal={The Astrophysical Journal},
The Gaia mission has opened a new window into the internal kinematics of young star clusters at the sub-km/s level, with implications for our understanding of how star clusters form and evolve. We use a sample of 28 clusters and associations with ages from 1-5 Myr, where lists of members are available from previous X-ray, optical, and infrared studies. Proper motions from Gaia DR2 reveals that at least 75% of these systems are expanding; however, rotation is only detected in one system. Typical… Expand
Gaia stellar kinematics in the head of the Orion A cloud: runaway stellar groups and gravitational infall
This work extends previous kinematic studies of young stars in the head of the Orion A cloud (OMC-1/2/3/4/5). It is based on large samples of infrared, optical, and X-ray selected pre-main-sequenceExpand
Not all stars form in clusters – Gaia-DR2 uncovers the origin of OB associations
Historically, it has often been asserted that most stars form in compact clusters. In this scenario, present-day gravitationally-unbound OB associations are the result of the expansion of initiallyExpand
A relation between the radial velocity dispersion of young clusters and their age
The majority of massive stars (> 8 M ) in OB associations are found in close binary systems. Nonetheless, the formation mechanism of these close massive binaries is not understood yet. UsingExpand
Untangling the Galaxy. I. Local Structure and Star Formation History of the Milky Way
Gaia DR2 provides unprecedented precision in measurements of the distance and kinematics of stars in the solar neighborhood. Through applying unsupervised machine learning on DR2's 5-dimensionalExpand
The Dynamical State of a Young Stellar Cluster
The dynamical state of the young star-forming cluster Rho Ophiuchi is considered, with emphasis on the L1688 cloud. Radial velocities are derived for 32 YSOs, with some being multi-epoch, usingExpand
The dynamics of the γ Vel cluster and nearby Vela OB2 association
The kinematics of low-mass stars in nearby OB associations can provide clues about their origins and evolution. Combining the precise positions, proper motions and parallaxes given in the second GaiaExpand
OB Associations and their origins
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 inExpand
Expanding associations in the Vela-Puppis region
Context. The Vela-Puppis region is known to host the Vela OB2 association as well as several young clusters featuring OB and pre-main-sequence stars. Several spatial and kinematic subgroups have beenExpand
IRAS 09002-4732: A Laboratory for the Formation of Rich Stellar Clusters
IRAS 09002-4732 is a poorly studied embedded cluster of stars in the Vela Molecular Ridge at a distance of 1.7kpc. Deep observations with the Chandra X-ray Observatory, combined with existing opticalExpand
A Kinematic Perspective on the Formation Process of the Stellar Groups in the Rosette Nebula
Stellar kinematics is a powerful tool for understanding the formation process of stellar associations. Here, we present a kinematic study of the young stellar population in the Rosette nebula usingExpand


Kinematics of NGC 2264: Signs of cluster formation
We present results from 1078 high-resolution spectra of 990 stars in the young open cluster NGC 2264, obtained with the Hectochelle multiobject echelle spectrograph on the 6.5 m MMT. We confirm 471Expand
The Gaia-ESO Survey: a kinematical and dynamical study of four young open clusters
Context. The origin and dynamical evolution of star clusters is an important topic in stellar astrophysics. Several models have been proposed in order to understand the formation of bound and unboundExpand
A Preliminary Study of the Orion Nebula Cluster Structure and Dynamics
We use optical and near-infrared star counts to explore the structure and dynamics of the Orion Nebula Cluster (ONC). This very young (<1 Myr) cluster is not circularly symmetric in projection but isExpand
Kinematic Signatures of Subvirial Initial Conditions in Young Clusters
Motivated by kinematic observations of young embedded clusters, this paper explores possible kinematic signatures produced by asphericity and departures from initial virial equilibrium in theseExpand
Radial-velocity measurements in 20 young open clusters
The further results of a program to determine the radial velocities of young open clusters are presented. Using the KPNO coude spectrograph coupled with the 1-m feed and 2.1-m telescopes, radialExpand
IN-SYNC. V. Stellar kinematics and dynamics in the Orion A Molecular Cloud
The kinematics and dynamics of young stellar populations enable us to test theories of star formation. With this aim, we continue our analysis of the SDSS-III/APOGEE IN-SYNC survey, a high resolutionExpand
Kinematic Structure of the Orion Nebula Cluster and Its Surroundings
We present results from 1351 high-resolution spectra of 1215 stars in the Orion Nebula Cluster (ONC) and the surrounding Orion 1c association, obtained with the Hectochelle multiobject echelleExpand
The Spatial Structure of Young Stellar Clusters. III. Physical Properties and Evolutionary States
We analyze the physical properties of stellar clusters that are detected in massive star-forming regions in the MYStIX project--a comparative, multiwavelength study of young stellar clusters withinExpand
The evolutionary tracks of young massive star clusters
Stars mostly form in groups consisting of a few dozen to several ten thousand members. For 30 years, theoretical models provide a basic concept of how such star clusters form and develop: theyExpand
The internal rotation of globular clusters revealed by Gaia DR2
Line-of-sight kinematic studies indicate that many Galactic globular clusters have a significant degree of internal rotation. However, three-dimensional kinematics from a combination of properExpand