Identification of emission-line stars in transition phase from pre-main sequence to main sequence

Pre-main sequence (PMS) stars evolve into main (MS) phase over a period of time. Interestingly, we found scarcity studies in existing literature that examines and attempts to better understand the PMS MS transition phase. The purpose present study is detect such rare stars, which named as 'Transition Phase' (TP) candidates - evolving from We identified 98 TP using photometric analysis sample 2167 classical Be (CBe) 225 Herbig Ae/Be (HAeBe) stars. This identification done by analyzing near- mid-infrared excess their location optical color-magnitude diagram. age mass 58 these are determined be between 0.1-5 Myr 2-10.5 M$_\odot$, respectively. possess rotational velocity color values CBe HAeBe reconfirmed generating set synthetic samples machine learning approach.