Franciosini, E, Sacco, GG, Jeffries, RD, Damiani, F, Roccatagliata, V, Fedele, D and Randich, S (2018) The Gaia DR2 view of the Gamma Velorum cluster: resolving the 6D structure. Astronomy & Astrophysics, 616. L12. ISSN 0004-6361

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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 ϖA = 2.895 ± 0.008 mas and ϖB = 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.

Item Type: Article
Additional Information: © EDP Sciences. This is the final published version of the article (version of record). It first appeared online via EDP Sciences at - please refer to any applicable terms of use of the publisher.
Uncontrolled Keywords: open clusters and associations: individual: Gamma Velorum / stars: late-type / stars: pre-main sequence / stars: distances / stars: kinematics and dynamics
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 10 Sep 2018 14:35
Last Modified: 30 Mar 2021 12:01

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