  Lee & Song (2018, Paper 1) 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 $\beta$
Pictoris moving group as a test case. In this study, we build models for all
major nearby young stellar moving groups (NYMGs hereafter) through 4 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 a NYMG changes, thus membership
probabilities change as well. A subset of stars show consistently large
membership probabilities regardless of the details of a chosen method for
ingesting additional members. Utilising these members, the NYMG models are
finalised. The finalised 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 BAMG and BANYAN
$\Sigma$ (Gagne et al. 2018b) are presented and discussed. Memberships of some
planet host stars are changed, and it can have a significant influence on the
estimated planetary masses.
