Travis Thieme (NTHU), Shih-Ping Lai (NTHU), Sheng-Jun Lin (NTHU), Pou-Ieng Cheong (NTHU), Ka Ho Lam (UVa), Zhi-Yun Li (UVa), Bo Zhao (MPE)
Understanding how material accretes to the rotationally supported disk from the surrounding envelope of gas and dust in the youngest protostellar systems is important for describing the environments in which these disks are formed. Magnetohydrodynamic simulations of magnetized, turbulent disk formation usually show spiral-like streams of material (accretion flows) connecting the envelope to the disk. However, observations of accretion flows in these early stages of protostellar formation still remain poorly characterized due to their low intensity. Here, we present our analysis of 12m ALMA archival data (C18O, 13CO, 12CO and SO) towards the young Class 0 source Lupus 3-MMS. We find that weighting the data to shorter baselines uncovers extended stream-like structures connecting to the disk plane. We isolate the spatial positions and velocity structures using a dendrogram algorithm and compare to a simple ballistic infall model, the CMU Model. We find that most of the streams are well-described by the CMU model, and also do not resemble velocity components of the molecular outflow.