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In the past years, high angular resolution observations have revealed thatcircumstellar discs appear in a variety of shapes with diverse substructuresbeing ubiquitous. This has given rise to the question of whether thesesubstructures are triggered by planet-disc interactions. Besides directimaging, one of the most promising methods to distinguish between differentdisc shaping mechanisms is to study the kinematics of the gas disc. Inparticular, the deviations of the rotation profile from Keplerian velocity canbe used to probe perturbations in the gas pressure profile that may be causedby embedded planets. In this paper we aim to analyze the gas brightnesstemperature and kinematics of the transitional disc around the CQ Tau star inorder to resolve and characterize substructure in the gas, caused by possibleperturbers. For our analysis we use spatially resolved ALMA observations of12CO, 13CO and C18O (J=2-1). We further extract robust line centroids for eachchannel map and fit a number of Keplerian disc models to the velocity field.The gas kinematics of the CQ Tau disc present non-Keplerian features, showingbent and twisted iso-velocity curves in 12CO and 13CO. Significant spiralstructures are detected between 10-180 au in both the brightness temperatureand the rotation velocity of 12CO after subtraction of an azimuthally symmetricmodel, which may be tracing planet-disc interactions with an embedded planet orlow-mass companion. We identify three spirals, two in the brightnesstemperature and one in the velocity residuals, spanning a large azimuth andradial extent. The brightness temperature spirals are morphologically connectedto spirals observed in NIR scattered light in the same disc, indicating acommon origin. Together with the observed large dust and gas cavity, thespirals support the hypothesis of a massive embedded companion in the CQ Taudisc.

A highly non-Keplerian protoplanetary disc: Spiral structure in the gas disc of CQ Tau