我們發現演化到後期的星體傾向疏散，遠離氣體，且他們的運動暗示著他們誕生於原本的地方而後驅散了周遭氣體。 而且我們分析過後，這個年輕星團正處於初步塌縮階段，而低質量核心很可能是快速移動的族群。;Most stars form in clusters embedded in giant molecular clouds and these systems are natural laboratories to study macrophysics of star formation. One way to get a comprehensive view of their star formation history is to concurrently study the two major components of these regions: young stellar objects (YSOs) and their natal molecular clouds. The $\rho$ Ophiuchus cloud complex, with its proximity ($\sim$138 pc) and a high concentration of gas and stellar population in infancy (1-2 Mys), is an excellent target for such a study.
Using the deepest 850$\mu$m JCMT/SCUBA-2 image of the densest core of $\rho$ Ophiuchus, generated as part of the JCMT Transient Survey, we trace the morphology of molecular clouds in the region. On the other hand, we also compiled a catalogue of YSOs in the region using published lists in literature and four more members, identified using the Gaia/eDR3 astrometric data. Using these datasets, we diagnosed the spatial and kinematic correlation of the young stellar population, at different evolutionary stages, with respect to the gaseous structures.
We found that the more evolved sources tend to be scattered further away from clouds and their kinematics suggest that they were formed in-situ and have dispersed the surrounding gas. Moreover, our analysis suggests that the young cluster is in the initial collapse phase and low mass cores are, likely, a faster-moving population.
