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We present a new method based on a Bayesian analysis to identify new membersof nearby young kinematic groups. The analysis minimally takes into account theposition, proper motion, magnitude and color of a star, but other observablescan be readily added (e.g. radial velocity, distance). We use this method tofind new young low-mass stars in the \beta Pictoris (\beta PMG) and AB Doradus(ABDMG) moving groups and in the TW Hydrae (TWA), Tucana-Horologium (THA),Columba, Carina and Argus associations. Starting from a sample of 758 mid-KM(K5V-M5V) stars showing youth indicators such as H\alpha\ and X-ray emission,our analysis yields 215 new highly probable low-mass members of the kinematicgroups analyzed. One is in TWA, 37 in \beta PMG, 17 in THA, 20 in Columba, 6 inCarina, 50 in Argus, 33 in ABDMG, and the remaining 51 candidates are likelyyoung but have an ambiguous membership to more than one association. The falsealarm rate for new candidates is estimated to be 5% for \beta PMG and TWA, 10%for THA, Columba, Carina and Argus, and 14% for ABDMG. Our analysis confirmsthe membership of 58 stars proposed in the literature. Firm membershipconfirmation of our new candidates will require measurement of their radialvelocity (predicted by our analysis), parallax and lithium 6708 {\AA}equivalent width. We have initiated these follow-up observations for a numberof candidates and we have identified two stars (2MASSJ0111+1526,2MASSJ0524-1601) as very strong candidate members of the \beta PMG and onestrong candidate member (2MASSJ0533-5117) of the THA; these three stars haveradial velocity measurements confirming their membership and lithium detectionsconsistent with young age. Finally, we proposed that six stars should beconsidered as new bona fide members of \beta PMG and ABDMG, one of which beingfirst identified in this work, the others being known candidates from theliterature.

Bayesian analysis to identify new star candidates in nearby young stellar kinematic groups