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We analyzed the archival data of the $^{13}\mathrm{CO}$ and$\mathrm{C}^{18}\mathrm{O}$ $J=3-2$ emission lines in the protoplanetary diskaround MWC 758 obtained with the Atacama Large Millimeter/submillimeter Arrayto discuss possible planet-disk interaction and non-Keplerian motion in thedisk. We performed fitting of a Keplerian disk model to the observational dataand measured the velocity deviations from the Keplerian rotation. We foundsignificant velocity deviations around the inner cavity in the MWC 758 disk. Weexamined several possibilities that may cause the velocity deviations, such aspressure gradient, height of the emitting layer, infall motion, inner warp, andeccentricity in the disk. We found that the combination of an eccentric orbitalmotion with eccentricity of $0.1\pm0.04$ at the radius of the inner cavity andan infalling flow best explains the observed velocity deviations. Ourkinematically constrained eccentricity of the gas orbital motion close to theinner cavity is consistent with the eccentricity of the dust ring around theinner cavity measured in the submillimeter continuum emission. Our results hintat strong dust-gas coupling around the inner cavity and presence of a gas giantplanet inside the inner cavity in the MWC 758 disk.

Kinematical Constraint on Eccentricity in the Protoplanetary Disk MWC 758 with ALMA