  We present Atacama Large Millimeter/sub-millimeter Array (ALMA) Cycle 2
observations of the 1.3 mm dust continuum emission of the protoplanetary disc
surrounding the T Tauri star Elias 24 with an angular resolution of $\sim 0.2"$
($\sim 28$ au). The dust continuum emission map reveals a dark ring at a radial
distance of $0.47"$ ($\sim 65$ au) from the central star, surrounded by a
bright ring at $0.58"$ ($\sim 81$ au). In the outer disc, the radial intensity
profile shows two inflection points at $0.71"$ and $0.87"$ ($\sim 99$ and $121$
au respectively). We perform global three-dimensional smoothed particle
hydrodynamic gas/dust simulations of discs hosting a migrating and accreting
planet. Combining the dust density maps of small and large grains with three
dimensional radiative transfer calculations, we produce synthetic ALMA
observations of a variety of disc models in order to reproduce the gap- and
ring-like features observed in Elias 24. We find that the dust emission across
the disc is consistent with the presence of an embedded planet with a mass of
$\sim 0.7\, \mathrm{M_{\mathrm{J}}}$ at an orbital radius of $\sim$ 60 au. Our
model suggests that the two inflection points in the radial intensity profile
are due to the inward radial motion of large dust grains from the outer disc.
The surface brightness map of our disc model provides a reasonable match to the
gap- and ring-like structures observed in Elias 24, with an average discrepancy
of $\sim$ 5% of the observed fluxes around the gap region.
