| In this dissertation I present a detailed survey of molecular line emission (including NH3, C2S, HC5N, N2H+, N2D+ and H 2D+) towards clustered star forming Cores in the nearby Ophiuchus molecular cloud, with the aim of characterizing the distribution and kinematics of the dense gas within a clustered star forming environment and compare these results with those found in more isolated star forming regions. I show that the dense Oph Cores present characteristics of both isolated and clustered star forming regions in several key parameters, including Core kinematics, temperatures and chemistry. At the higher gas densities where the N2 H+ emission is excited, I show that the presence of an embedded protostar is correlated with increased gas motions. I additionally present evidence of N2H+ depletion from the gas phase, suggesting that in higher density, clustered environments N2H + may not accurately trace the physical conditions of the densest core gas. I present the distribution of H2D+ and N2D+ across the Oph B Core, and show the distribution is not simple or easily explained by chemical models of evolving, isolated cores. Finally, I summarize the results of this dissertation, the questions it raises concerning the exploration of how stars form in clusters, and discuss how these questions may be answered through upcoming observational surveys and by new telescope facilities. |
