  Recent mm-wavelength surveys performed with the Atacama Large Millimeter
Array (ALMA) have revealed protoplanetary discs characterized by rings and
gaps. A possible explanation for the origin of such rings is the tidal
interaction with an unseen planetary companion. The protoplanetary disc around
DS Tau shows a wide gap in the ALMA observation at 1.3 mm. We construct a
hydrodynamical model for the dust continuum observed by ALMA assuming the
observed gap is carved by a planet between one and five Jupiter masses. We fit
the shape of the radial intensity profile along the disc major axis varying the
planet mass, the dust disc mass, and the evolution time of the system. The best
fitting model is obtained for a planet with $M_{\rm p}=3.5\,M_{\rm Jup}$ and a
disc with $M_{\rm dust}= 9.6\cdot10^{-5}\,M_{\odot}$. Starting from this
result, we also compute the expected signature of the planet in the gas
kinematics, as traced by CO emission. We find that such a signature (in the
form of a "kink" in the channel maps) could be observed by ALMA with a velocity
resolution between $0.2-0.5\,\rm{kms}^{-1}$ and a beam size between 30 and 50
mas.
