Internal Dynamics and Membership of the NGC 3603 Young Cluster From Microarcsecond Astrometry

Rochau, Boyke; Brandner, W.; Stolte, A.; Gennaro, Mario; Gouliermis, D. A.; Rio, Nicola Da; Dzyurkevich, Natalia; Henning, Thomas

doi:10.1088/2041-8205/716/1/l90

Cited by 87 publications

(124 citation statements)

References 32 publications

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“…Proper motions provide kinematic information of stars, which is often a very useful discriminant to separate members of a cluster or stellar association from unrelated field objects (see, A15, page 4 of 17 e.g., Rochau et al 2010). Recently, Röser et al (2010) presented a new catalog of proper motions based on the International Celestial Reference System (ICRS) using a combination of USNO-B1.0 and 2MASS astrometry.…”

Section: Proper Motionsmentioning

confidence: 99%

Young stars inϵChamaleontis and their disks: disk evolution in sparse associations

Fang

Boekel

Bouwman

et al. 2012

A&A

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Context. The nearby young stellar association Cha has an estimated age of 3-5 Myr, making it an ideal laboratory to study the disk dissipation process and provide empirical constraints on the timescale of planet formation. Aims. We wish to complement existing optical and near-infrared data of the Cha association, which provide the stellar properties of its members, with mid-infrared data that probe the presence, geometry, and mineralogical composition of protoplanetary disks around individual stars. Methods. We combine the available literature data with our Spitzer/IRS spectroscopy and VLT/VISIR imaging data. We use proper motions to refine the membership of Cha. Masses and ages of individual stars are estimated by fitting model atmospheres to the optical and near-infrared photometry, followed by placement in the Hertzsprung-Russell diagram. The Spitzer/IRS spectra are analyzed using the two-layer temperature distribution spectral decomposition method. Results. Two stars previously identified as members, CXOU J120152.8 and 2MASS J12074597, have proper motions that are very different from those of the other stars. But other observations suggest that the two stars are still young and thus might still be related to Cha. HD 104237C is the lowest mass member of Cha with an estimated mass of ∼13-15 Jupiter masses. The very low mass stars USNO-B120144.7 and 2MASS J12005517 show globally depleted spectral energy distributions, pointing at strong dust settling. 2MASS J12014343 may have a disk with a very specific inclination, where the central star is effectively screened by the cold outer parts of a flared disk, but the 10 μm radiation of the warm inner disk can still reach us. We find that the disks in sparse stellar associations are dissipated more slowly than those in denser (cluster) environments. We detect C 2 H 2 rovibrational band around 13.7 μm on the IRS spectrum of USNO-B120144.7. We find strong signatures of grain growth and crystallization in all Cha members with 10 μm features detected in their IRS spectra. We combine the dust properties derived in the Cha sample with those found using identical or similar methods in the MBM 12, Coronet, η Cha associations, and in the cores-to-disks legacy program. We find that disks around low-mass young stars show a negative radial gradient in the mass-averaged grain size and mass fraction of crystalline silicates. A positive correlation exists between the mass-averaged grain sizes of amorphous silicates and the accretion rates if the latter is above ∼10 −9 M yr −1 , possibly indicating that those disks are sufficiently turbulent to prevent grains of several microns in size to sink into the disk interior.

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Section: Proper Motionsmentioning

confidence: 99%

Young stars inϵChamaleontis and their disks: disk evolution in sparse associations

Fang

Boekel

Bouwman

et al. 2012

A&A

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“…The velocity dispersion of 0.72 ± 0.07 km s −1 implies a super-virial dynamical state. More massive clusters such as Westerlund I, NGC 3603, and R136 have been studied by Cottaar et al (2012), Rochau et al (2010), and Hénault-Brunet et al (2012), respectively. Kinematic studies for the Orion Nebula Cluster (ONC) and NGC 2264 also exist (Furesz et al 2006;Furesz et al 2008;Tobin et al 2015), together with studies of Cyg OB2 .…”

Section: Introductionmentioning

confidence: 99%

TheGaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

Rigliaco

Wilking

Meyer

et al. 2016

A&A

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The Gaia ESO Public Spectroscopic Survey (GES) is providing the astronomical community with high-precision measurements of many stellar parameters including radial velocities (RVs) of stars belonging to several young clusters and star-forming regions. One of the main goals of the young cluster observations is to study their dynamical evolution and provide insight into their future, revealing whether they will eventually disperse to populate the field rather than evolve into bound open clusters. In this paper we report the analysis of the dynamical state of L1688 in the ρ Ophiuchi molecular cloud using the dataset provided by the GES consortium. We performed the membership selection of the more than 300 objects observed. Using the presence of the lithium absorption and the location in the Hertzspung-Russell diagram, we identify 45 already known members and two new association members. We provide accurate RVs for all 47 confirmed members. A dynamical analysis, after accounting for unresolved binaries and errors, shows that the stellar surface population of L1688 has a velocity dispersion σ ∼ 1.14 ± 0.35 km s −1 that is consistent with being in virial equilibrium and is bound with a ∼80% probability. We also find a velocity gradient in the stellar surface population of ∼1.0 km s −1 pc −1 in the northwest-southeast direction, which is consistent with that found for the pre-stellar dense cores, and we discuss the possibility of sequential and triggered star formation in L1688.

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“…This theory of cluster disruption, often referred to as residual gas expulsion, predicts that a large fraction of young and non-embedded star clusters should be supervirial and in the process of expanding. However most kinematic observations of exposed star clusters have shown them to be in (or close to) virial equilibrium (e.g., Rochau et al, 2010;Hénault-Brunet et al, 2012;Cottaar et al, 2012). This raises the question of why gas expulsion hasn't influenced the virial state of these clusters?…”

Section: The Role Of Kinematics In the Formation Of Star Clustersmentioning

confidence: 99%

Star formation in the Gaia era

Wright

2016

A&G

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The European Space Agency's Gaia space telescope, launched in 2013, aims to measure the positions, parallaxes, and proper motions of a billion stars in our Galaxy and throughout the Local Group. In doing so it will include hundreds of thousands of young stars in star forming regions, star clusters and OB associations. This will provide us with an unprecedented view of the role of dynamics in the star formation process and the evolution of young star clusters. Data from this ambitious mission is expected very soon, with the first data release scheduled for 2016. This review discusses the current state of our understanding of the kinematics of star formation and how the community can best prepare for Gaia data.

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Internal Dynamics and Membership of the NGC 3603 Young Cluster From Microarcsecond Astrometry

Cited by 87 publications

References 32 publications

Young stars inϵChamaleontis and their disks: disk evolution in sparse associations

Young stars inϵChamaleontis and their disks: disk evolution in sparse associations

TheGaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

Star formation in the Gaia era

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