A highly non-Keplerian protoplanetary disc

In the past years, high angular resolution observations have revealed that circumstellar discs appear in a variety of shapes with diverse substructures being ubiquitous. This has given rise to question whether these are triggered by planet-disc interactions. Besides direct imaging, one most promising methods distinguish between different disc shaping mechanisms is study kinematics gas disc. particular, deviations rotation profile from Keplerian velocity can be used probe perturbations pressure may caused embedded planets. this paper we aim analyze brightness temperature and transitional around CQ Tau star order resolve characterize substructure gas, possible perturbers. For our analysis use spatially resolved ALMA 12CO, 13CO C18O (J=2-1). We further extract robust line centroids for each channel map fit number models field. The present non-Keplerian features, showing bent twisted iso-velocity curves 12CO 13CO. Significant spiral structures detected 10-180 au both after subtraction an azimuthally symmetric model, which tracing interactions planet or low-mass companion. identify three spirals, two residuals, spanning large azimuth radial extent. spirals morphologically connected observed NIR scattered light same disc, indicating common origin. Together dust cavity, support hypothesis massive companion