The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster

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The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster. / Jeffries, R. D.; Jackson, R. J.; Cottaar, M.; Koposov, S. E.; Lanzafame, A. C.; Meyer, M. R.; Prisinzano, L.; Randich, S.; Sacco, G. G.; Brugaletta, E.; Caramazza, M.; Damiani, F.; Franciosini, E.; Frasca, A.; Gilmore, G.; Feltzing, Sofia; Micela, G.; Alfaro, E.; Bensby, Thomas; Pancino, E.; Recio-Blanco, A.; De laverny, P.; Lewis, J.; Magrini, L.; Morbidelli, L.; Costado, M. T.; Jofre, P.; Klutsch, A.; Lind, K.; Maiorca, E.

In: Astronomy & Astrophysics, Vol. 563, A94, 2014.

Research output: Contribution to journalArticle

Harvard

Jeffries, RD, Jackson, RJ, Cottaar, M, Koposov, SE, Lanzafame, AC, Meyer, MR, Prisinzano, L, Randich, S, Sacco, GG, Brugaletta, E, Caramazza, M, Damiani, F, Franciosini, E, Frasca, A, Gilmore, G, Feltzing, S, Micela, G, Alfaro, E, Bensby, T, Pancino, E, Recio-Blanco, A, De laverny, P, Lewis, J, Magrini, L, Morbidelli, L, Costado, MT, Jofre, P, Klutsch, A, Lind, K & Maiorca, E 2014, 'The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster', Astronomy & Astrophysics, vol. 563, A94. https://doi.org/10.1051/0004-6361/201323288

APA

Jeffries, R. D., Jackson, R. J., Cottaar, M., Koposov, S. E., Lanzafame, A. C., Meyer, M. R., Prisinzano, L., Randich, S., Sacco, G. G., Brugaletta, E., Caramazza, M., Damiani, F., Franciosini, E., Frasca, A., Gilmore, G., Feltzing, S., Micela, G., Alfaro, E., Bensby, T., ... Maiorca, E. (2014). The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster. Astronomy & Astrophysics, 563, [A94]. https://doi.org/10.1051/0004-6361/201323288

CBE

Jeffries RD, Jackson RJ, Cottaar M, Koposov SE, Lanzafame AC, Meyer MR, Prisinzano L, Randich S, Sacco GG, Brugaletta E, Caramazza M, Damiani F, Franciosini E, Frasca A, Gilmore G, Feltzing S, Micela G, Alfaro E, Bensby T, Pancino E, Recio-Blanco A, De laverny P, Lewis J, Magrini L, Morbidelli L, Costado MT, Jofre P, Klutsch A, Lind K, Maiorca E. 2014. The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster. Astronomy & Astrophysics. 563:Article A94. https://doi.org/10.1051/0004-6361/201323288

MLA

Vancouver

Jeffries RD, Jackson RJ, Cottaar M, Koposov SE, Lanzafame AC, Meyer MR et al. The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster. Astronomy & Astrophysics. 2014;563. A94. https://doi.org/10.1051/0004-6361/201323288

Author

Jeffries, R. D. ; Jackson, R. J. ; Cottaar, M. ; Koposov, S. E. ; Lanzafame, A. C. ; Meyer, M. R. ; Prisinzano, L. ; Randich, S. ; Sacco, G. G. ; Brugaletta, E. ; Caramazza, M. ; Damiani, F. ; Franciosini, E. ; Frasca, A. ; Gilmore, G. ; Feltzing, Sofia ; Micela, G. ; Alfaro, E. ; Bensby, Thomas ; Pancino, E. ; Recio-Blanco, A. ; De laverny, P. ; Lewis, J. ; Magrini, L. ; Morbidelli, L. ; Costado, M. T. ; Jofre, P. ; Klutsch, A. ; Lind, K. ; Maiorca, E. / The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster. In: Astronomy & Astrophysics. 2014 ; Vol. 563.

RIS

TY - JOUR

T1 - The Gaia-ESO Survey: Kinematic structure in the Gamma Velorum cluster

AU - Jeffries, R. D.

AU - Jackson, R. J.

AU - Cottaar, M.

AU - Koposov, S. E.

AU - Lanzafame, A. C.

AU - Meyer, M. R.

AU - Prisinzano, L.

AU - Randich, S.

AU - Sacco, G. G.

AU - Brugaletta, E.

AU - Caramazza, M.

AU - Damiani, F.

AU - Franciosini, E.

AU - Frasca, A.

AU - Gilmore, G.

AU - Feltzing, Sofia

AU - Micela, G.

AU - Alfaro, E.

AU - Bensby, Thomas

AU - Pancino, E.

AU - Recio-Blanco, A.

AU - De laverny, P.

AU - Lewis, J.

AU - Magrini, L.

AU - Morbidelli, L.

AU - Costado, M. T.

AU - Jofre, P.

AU - Klutsch, A.

AU - Lind, K.

AU - Maiorca, E.

PY - 2014

Y1 - 2014

N2 - 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 gamma(2) Velorum was one of the first GES targets. 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 angstrom 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(-1) and sufficient to resolve velocity structure in the low-mass population around gamma(2) Vel. The structure is well fitted by two kinematic components with roughly equal numbers of stars; the first has an intrinsic dispersion of 0.34 +/- 0.16 km s(-1), consistent with virial equilibrium. The second has a broader dispersion of 1.60 +/- 0.37 km s(-1) and is offset from the first by congruent to 2 kms(-1). The first population is older by 1-2 Myr based on a greater level of Li depletion seen among its M-type stars and is probably more centrally concentrated around gamma(2) Vel. Conclusions. We consider several formation scenarios, concluding that the two kinematic components are a bound remnant of the original, denser cluster that formed gamma(2) Vel, and a dispersed population from the wider Vela OB2 association, of which gamma(2) Vel is the most massive member. The apparent youth of gamma(2) Vel compared to the older (>= 10 Myr) low-mass population surrounding it suggests a scenario in which the massive binary formed in a clustered environment after the formation of the bulk of the low-mass stars.

AB - 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 gamma(2) Velorum was one of the first GES targets. 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 angstrom 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(-1) and sufficient to resolve velocity structure in the low-mass population around gamma(2) Vel. The structure is well fitted by two kinematic components with roughly equal numbers of stars; the first has an intrinsic dispersion of 0.34 +/- 0.16 km s(-1), consistent with virial equilibrium. The second has a broader dispersion of 1.60 +/- 0.37 km s(-1) and is offset from the first by congruent to 2 kms(-1). The first population is older by 1-2 Myr based on a greater level of Li depletion seen among its M-type stars and is probably more centrally concentrated around gamma(2) Vel. Conclusions. We consider several formation scenarios, concluding that the two kinematic components are a bound remnant of the original, denser cluster that formed gamma(2) Vel, and a dispersed population from the wider Vela OB2 association, of which gamma(2) Vel is the most massive member. The apparent youth of gamma(2) Vel compared to the older (>= 10 Myr) low-mass population surrounding it suggests a scenario in which the massive binary formed in a clustered environment after the formation of the bulk of the low-mass stars.

KW - stars: pre-main sequence

KW - stars: kinematics and dynamics

KW - open clusters

KW - and associations: individual: gamma2 Velorum

KW - stars: formation

U2 - 10.1051/0004-6361/201323288

DO - 10.1051/0004-6361/201323288

M3 - Article

VL - 563

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 1432-0746

M1 - A94

ER -