Physical parameters of pre-main sequence stars in open clusters

TL;DR

This paper determines physical parameters of pre-main sequence stars in young open clusters by comparing photometric data with theoretical models, validating methods for membership and parameter estimation.

Contribution

It introduces a comparative approach using multiple model isochrones to accurately determine stellar parameters and membership in young open clusters.

Findings

Successful membership assignment for MS and PMS stars

Consistent relations between cluster parameters

Validated methodology for physical parameter estimation

Abstract

Our aims are twofold: To determine the physical parameters of PMS members in young open clusters (YOCs), and to check and compare the performances of different model isochrones. We compare UBVRI photometric observations of YOCs to theoretical isochrones in the photometric diagrams. The comparison simultaneously provides membership assignments for MS and PMS stars, and estimates for the masses, ages, and spatial distribution of the candidate members. The relations found between the different cluster parameters show that the procedure applied to assign cluster membership, and to measure physical parameters for the selected members, is well founded.