The Keele-Exeter young cluster survey: I. Low mass pre-main sequence stars in NGC 2169

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dc.creatorJeffries, R. D
dc.creatorOliveira, J. M.
dc.creatorNaylor, Tim
dc.creatorMayne, N. J.
dc.creatorLittlefair, S. P.
dc.date2006-11-20
dc.date.accessioned2026-07-07T10:20:55Z
dc.date.available2026-07-07T10:20:55Z
dc.descriptionWe have used R_C I_C CCD photometry from the Isaac Newton telescope and intermediate resolution spectroscopy from the Gemini North telescope to identify and characterise low-mass (0.15<M/M_sun<1.3) pre-main sequence stars in the young open cluster NGC 2169. Isochrone fitting to the high- and low-mass populations yields an intrinsic distance modulus of 10.13{+0.06}{-0.09} mag and a model-dependent age of 9+/-2 Myr. Compared with the nearby, kinematically defined groups of a similar age, NGC 2169 has a large low-mass population which potentially offers a more precise statistical investigation of several aspects of star formation and early stellar evolution. By modelling the distribution of low-mass stars in the I_C versus R_C-I_C diagram we find that any age spread among cluster members has a Gaussian full width at half maximum <=2.5 Myr. A young age and small age spread (<10 Myr) are supported by the lack of significant lithium depletion in the vast majority of cluster members. There is no clear evidence for accretion or warm circumstellar dust in the low-mass members of NGC 2169, bolstering the idea that strong accretion has ceased and inner discs have dispersed in almost all low-mass stars by ages of 10 Myr.
dc.descriptionAccpted for publication in MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0611630
dc.identifierhttp://arxiv.org/abs/astro-ph/0611630
dc.identifierMon.Not.Roy.Astron.Soc.376:580-598,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11327.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175003
dc.subjectAstrophysics
dc.titleThe Keele-Exeter young cluster survey: I. Low mass pre-main sequence stars in NGC 2169
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