Volume 589, May 2016
|Number of page(s)||14|
|Section||Galactic structure, stellar clusters and populations|
|Published online||14 April 2016|
INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento
2 Astrophysics Group, Keele University, Keele, Staffordshire ST5 5BG, UK
3 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Florence, Italy
4 INAF–Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy
5 Dipartimento di Fisica e Astronomia, Università di Catania, via S. Sofia 78, 95123 Catania, Italy
6 Instituto de Astrofísica de Andalucía-CSIC, Apdo. 3004, 18080 Granada, Spain
7 Dip. di Fisica e Chimica, Università di Palermo, P.zza del Parlamento 1, 90134 Palermo, Italy
8 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy
9 INAF–Padova Observatory, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
10 European Southern Observatory, Alonso de Cordova 3107 Vitacura, Santiago de Chile, Chile
11 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
12 Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK
13 Departamento de Ciencias Fisicas, Universidad Andres Bello, Republica 220, Santiago, Chile
14 Department of Astronomy, University of Geneva, 51 chemin des Maillettes, 1290 Versoix, Switzerland
Received: 1 December 2015
Accepted: 21 January 2016
Context. Understanding the properties of young open clusters, such as the initial mass function (IMF), star formation history, and dynamic evolution, is crucial for obtaining reliable theoretical predictions of the mechanisms involved in the star formation process.
Aims. We want to obtain a list that is as complete as possible of confirmed members of the young open cluster γ Velorum, with the aim of deriving general cluster properties such as the IMF.
Methods. We used all available spectroscopic membership indicators within the Gaia-ESO public archive, together with literature photometry and X-ray data, and for each method, we derived the most complete list of candidate cluster members. Then, we considered photometry, gravity, and radial velocities as necessary conditions for selecting a subsample of candidates whose membership was confirmed by using the lithium and Hα lines and X-rays as youth indicators.
Results. We found 242 confirmed and 4 possible cluster members for which we derived masses using very recent stellar evolutionary models. The cluster IMF in the mass range investigated in this study shows a slope of α = 2.6 ± 0.5 for 0.5 <M/M⊙< 1.3 and α = 1.1 ± 0.4 for 0.16 <M/M⊙< 0.5, and it is consistent with a standard IMF.
Conclusions. The similarity of the IMF of the young population around γ2Vel to that in other star-forming regions and the field suggests it may have formed through very similar processes.
Key words: stars: pre-main sequence / open clusters and associations: individual: γVelorum / stars: formation / stars: luminosity function, mass function / techniques: radial velocities / techniques: spectroscopic
Based on observations made with the ESO/VLT, at Paranal Observatory under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey).
Table 5 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/589/A70
© ESO, 2016
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