dc.contributor.author | Jeffries, RD | |
dc.contributor.author | Naylor, T | |
dc.contributor.author | Walter, FM | |
dc.contributor.author | Pozzo, MP | |
dc.contributor.author | Devey, CR | |
dc.date.accessioned | 2017-06-20T08:12:44Z | |
dc.date.issued | 2009-02-01 | |
dc.description.abstract | We present the results of a photometric BVI survey of 0.9deg<SUP>2</SUP> around the Wolf-Rayet binary gamma<SUP>2</SUP> Vel and its early-type common proper motion companion gamma<SUP>1</SUP> Vel (together referred to as the gamma 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, Halpha emission and high levels of X-ray activity. We show that the PMS stars are kinematically coherent and spatially concentrated around gamma Vel. The PMS stars have similar proper motions to gamma Vel, to main-sequence (MS) stars around gamma Vel and to early-type stars of the wider Vela OB2 association of which gamma<SUP>2</SUP> Vel is the brightest member. The ratio of MS stars to low-mass (0.1-0.6M<SUB>solar</SUB>) PMS stars is consistent with a Kroupa mass function. MS fitting to stars around gamma Vel gives an association distance modulus of 7.76 +/- 0.07mag, which is consistent with a similarly determined distance for Vela OB2 and also with interferometric distances to gamma<SUP>2</SUP> Vel. High-mass stellar models indicate an age of 3-4Myr for gamma<SUP>2</SUP> Vel, but the low-mass PMS stars have ages of ~=10Myr according to low-mass evolutionary models and 5-10Myr 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 gamma Vel, and this is a subcluster within the larger Vela OB2 association. We speculate that gamma<SUP>2</SUP> 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. | en_GB |
dc.identifier.citation | Vol. 393, pp. 538 - 556 | en_GB |
dc.identifier.doi | 10.1111/j.1365-2966.2008.14162.x | |
dc.identifier.uri | http://hdl.handle.net/10871/28101 | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press (OUP) / Royal Astronomical Society | en_GB |
dc.relation.url | http://adsabs.harvard.edu/abs/2009MNRAS.393..538J | en_GB |
dc.subject | stars: formation | en_GB |
dc.subject | stars: pre-main-sequence | en_GB |
dc.subject | stars: Wolf-Rayet | en_GB |
dc.subject | open clusters and associations: individual: Vela OB2 | en_GB |
dc.title | The stellar association around Gamma Velorum and its relationship with Vela OB2 | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2017-06-20T08:12:44Z | |
dc.identifier.issn | 0035-8711 | |
dc.description | This is the author accepted manuscript. The final version is available from the publisher via the DOI in this record. | en_GB |
dc.identifier.journal | Monthly Notices of the Royal Astronomical Society | en_GB |