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dc.rights.license© P. A. B. Galli et al. 2021es
dc.contributor.authorGalli, P. A. B.-
dc.contributor.authorBouy, H.-
dc.contributor.authorOlivares, J.-
dc.contributor.authorMiret Roig, N.-
dc.contributor.authorSarro, L. M.-
dc.contributor.authorBarrado, D.-
dc.contributor.authorBerihuete, A.-
dc.contributor.authorBertín, E.-
dc.contributor.authorCuillandre, J. C.-
dc.identifier.citationAstronomy and Astrophysics 646: A46(2021)es
dc.descriptionFull Tables A.1–A.7 are only available at the CDS via anonymous ftp to ( or via
dc.description.abstractContext. Chamaeleon is the southernmost low-mass star-forming complex within 200 pc from the Sun. Its stellar population has been extensively studied in the past, but the current census of the stellar content is not complete yet and deserves further investigation. Aims. We take advantage of the second data release of the Gaia space mission to expand the census of stars in Chamaeleon and to revisit the properties of the stellar populations associated to the Chamaeleon I (Cha I) and Chamaeleon II (Cha II) dark clouds. Methods. We perform a membership analysis of the sources in the Gaia catalogue over a field of 100 deg2 encompassing the Chamaeleon clouds, and use this new census of cluster members to investigate the 6D structure of the complex. Results. We identify 188 and 41 high-probability members of the stellar populations in Cha I and Cha II, respectively, including 19 and 7 new members. Our sample covers the magnitude range from G = 6 to G = 20 mag in Cha I, and from G = 12 to G = 18 mag in Cha II. We confirm that the northern and southern subgroups of Cha I are located at different distances (191.4−0.8+0.8 pc and 186.7−1.0+1.0 pc), but they exhibit the same space motion within the reported uncertainties. Cha II is located at a distance of 197.5−0.9+1.0 pc and exhibits a space motion that is consistent with Cha I within the admittedly large uncertainties on the spatial velocities of the stars that come from radial velocity data. The median age of the stars derived from the Hertzsprung-Russell diagram and stellar models is about 1−2 Myr, suggesting that they are somewhat younger than previously thought. We do not detect significant age differences between the Chamaeleon subgroups, but we show that Cha II exhibits a higher fraction of disc-bearing stars compared to Cha I. Conclusions. This study provides the most complete sample of cluster members associated to the Chamaeleon clouds that can be produced with Gaia data alone. We use this new census of stars to revisit the 6D structure of this region with unprecedented
dc.description.sponsorshipWe thank the referee for constructive criticism that improved the manuscript. This research has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 682903, P.I. H. Bouy), and from the French State in the framework of the Investments for the future Program, IdEx Bordeaux, reference ANR-10-IDEX-03-02. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (, processed by the Gaia Data Processing and Analysis Consortium (DPAC, for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of data products from theWidefield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space
dc.publisherEDP Scienceses
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.subjectOpen Clusterses
dc.subjectAssociations: individual: Chamaeleones
dc.subjectStars: formationes
dc.subjectStars: distanceses
dc.subjectMethods: statisticalses
dc.subjectProper motionses
dc.titleChamaeleon DANCe Revisiting the stellar populations of Chamaeleon I and Chamaeleon II with Gaia-DR2 dataes
dc.contributor.orcidBerihuete, A. [0000-0002-8589-4423]-
dc.contributor.orcidGalli, P. A. B. [0000-0003-2271-9297]-
dc.contributor.orcidOlivares Romero, J. [0000-0003-0316-2956]-
dc.contributor.funderEuropean Research Council (ERC)-
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