The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster$^{⋆,⋆⋆}$
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Abstract
Context. A key science goal of the Gaia-ESO survey (GES) at the VLT is to use the kinematics of low-mass stars in young clusters and star forming regions to probe their dynamical histories and how they populate the field as they become unbound. The clustering of low-mass stars around the massive Wolf-Rayet binary system γ
Aims. We empirically determine the radial velocity precision of GES data, construct a kinematically unbiased sample of cluster members and characterise their dynamical state.
Methods. Targets were selected from colour–magnitude diagrams and intermediate resolution spectroscopy was used to derive radial velocities and assess membership from the strength of the Li i 6708 Å line. The radial velocity distribution was analysed using a maximum likelihood technique that accounts for unresolved binaries.
Results. The GES radial velocity precision is about 0.25 km s
Conclusions. We consider several formation scenarios, concluding that the two kinematic components are a bound remnant of the original, denser cluster that formed γ
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1432-0746
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Science and Technology Facilities Council (ST/J00541X/1)
Science and Technology Facilities Council (ST/L001381/1)
European Research Council (320360)
European Commission (264895)