Abstract
Abstract The disk around MWC 480 has shown multiple substructures in both dust and gas observations, possibly suggesting ongoing planet formation in situ. In this paper, we explore the gas kinematics of the MWC 480 disk by analyzing the archival Atacama Large (sub-) Millimetre Array observations of $^{12}$CO (J = 2-1), $^{13}$CO (J = 2-1), and C$^{18}$O (J = 2-1). By modeling the line-of-sight velocities, inferred from the Doppler shifts of the emission lines, we are able to decompose the 3-D velocity field of the disk into rotational, radial, and vertical components. Further analysis reveals the presence of large-scale gas flows in the $(\mathit{r}, \mathit{z})$ plane. Notably, we identify potential meridional flows across various heights as traced by all three CO isotopologues in the 80-120 au region, possibly associated with ongoing planet formation activities in this region. Moreover, we find that upward flows near 200 au for all three CO isotopologues, which may point to the presence of disk winds.
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