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The Gaia DR2 view of the Gamma Velorum cluster: resolving the 6D structure

Franciosini, E.; Sacco, G.G.; Jeffries, R.D.; Damiani, F.; Roccatagliata, V.; Fedele, D.; Randich, S.

The Gaia DR2 view of the Gamma Velorum cluster: resolving the 6D structure Thumbnail


Authors

E. Franciosini

G.G. Sacco

F. Damiani

V. Roccatagliata

D. Fedele

S. Randich



Abstract

Gaia-ESO Survey observations of the young Gamma Velorum cluster led to the discovery of two kinematically distinct populations, Gamma Vel A and B, respectively, with population B extended over several square degrees in the Vela OB2 association. Using the Gaia DR2 data for a sample of high-probability cluster members, we find that the two populations differ not only kinematically, but are also located at different distances along the line of sight, with the main cluster Gamma Vel A being closer. A combined fit of the two populations yields ?A = 2.895 ± 0.008 mas and ?B = 2.608 ± 0.017 mas, with intrinsic dispersions of 0.038 ± 0.011 mas and 0.091 ± 0.016 mas, respectively. This translates into distances of 345.4+1.0+12.4-1.0-11.5 pc and 383.4+2.5+15.3-2.5-14.2 pc, respectively, showing that Gamma Vel A is closer than Gamma Vel B by ~38 pc. We find that the two clusters are nearly coeval, and that Gamma Vel B is expanding. We suggest that Gamma Vel A and B are two independent clusters located along the same line of sight.

Journal Article Type Letter
Acceptance Date Aug 13, 2018
Online Publication Date Aug 22, 2018
Publication Date Aug 22, 2018
Publicly Available Date Mar 29, 2024
Journal Astronomy & Astrophysics
Print ISSN 0004-6361
Publisher EDP Sciences
Peer Reviewed Peer Reviewed
Volume 616
Pages L12
DOI https://doi.org/10.1051/0004-6361/201833815
Keywords open clusters and associations: individual: Gamma Velorum / stars: late-type / stars: pre-main sequence / stars: distances / stars: kinematics and dynamics
Publisher URL http://dx.doi.org/10.1051/0004-6361/201833815

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