Development of models for nearbaby young stellar moving groups: creation, revision, and finalization of the models

In our previous research, we developed a tool for calculating Bayesian membership probability for nearby young stellar moving groups (BAMG: Bayesian Analysis of Moving Groups). The study presented the importance of careful construction of models in moving group membership assessment, using β Pictoris moving group as a test case. In this study, we build models for all major nearby young stellar moving groups (NYMGs hereafter) through four stages. A set of prototype models is created using members listed in the discovery paper of each group. For each group, suggested members after the discovery of the group are used for revising these prototype models. As these additional members being incorporated, group properties of an NYMG changes, thus membership probabilities change as well. A subset of stars shows consistently large membership probabilities regardless of the details of a chosen method for ingesting additional members. Utilizing these members, the NYMG models are finalized. The finalized models are applied for evaluating memberships of all claimed candidate members, resulting in a list of bona fide members. The mass function of bona fide members for the entire set of NYMG members indicates that more late M-type members should be identified. In addition, some objects showing a large difference in membership probability between this study and the other study are presented and discussed. Memberships of some planet host stars are changed, and it can have a significant influence on the estimated planetary masses.