• DOI:10.1111/j.1365-2966.2008.14162.x
• Corpus ID: 17560818

The stellar association around Gamma Velorum and its relationship with Vela OB2

@article{Jeffries2009TheSA,
  title={The stellar association around Gamma Velorum and its relationship with Vela OB2},
  author={R D Jeffries and Tim Naylor and Frederick M. Walter and Monica Pozzo and Cambridge University and University of Exeter and Suny and Stony Brook and University College and London},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2009},
  volume={393},
  pages={538-556}
}

• R. Jeffries, T. Naylor, +7 authors London
• Published 29 October 2008
• Physics
• Monthly Notices of the Royal Astronomical Society

We present the results of a photometric BVI survey of 0.9 deg 2 around the Wolf-Rayet binary γ 2 Vel and its early-type common proper motion companion γ 1 Vel (together referred to as the y Vel system). Several hundred pre-main-sequence (PMS) stars are identified and the youth of a subset of these is spectroscopically confirmed by the presence of lithium in their atmospheres, Ha emission and high levels of X-ray activity. We show that the PMS stars are kinematically coherent and spatially concentrated around y Vel. The PMS stars have similar proper motions to y Vel, to main-sequence (MS) stars around y Vel and to early-type stars of the wider Vela OB2 association of which γ 2 Vel is the brightest member. The ratio of MS stars to low-mass (0.1-0.6M ⊙ ) PMS stars is consistent with a Kroupa mass function. MS fitting to stars around y Vel gives an association distance modulus of 7.76 ± 0.07 mag, which is consistent with a similarly determined distance for Vela OB2 and also with interferometric distances to γ 2 Vel. High-mass stellar models indicate an age of 3-4Myr for γ 2 Vel, but the low-mass PMS stars have ages of ≃10 Myr according to low-mass evolutionary models and 5-10 Myr by empirically placing them in an age sequence with other clusters based on colour-magnitude diagrams and lithium depletion. We conclude that the low-mass PMS stars form a genuine association with y Vel, and this is a subcluster within the larger Vela OB2 association. We speculate that γ 2 Vel formed after the bulk of the low-mass stars, expelling gas, terminating star formation and unbinding the association. The velocity dispersion of the PMS stars is too low for this star-forming event to have produced all the stars in the extended Vela OB2 association. Instead, star formation must have been initiated at several sites within a molecular cloud either sequentially or simultaneously after some triggering event.