  We present high angular-resolution observations of Sakurai's object using the
Atacama Large Millimeter Array, shedding new light on its morpho-kinematical
structure. The millimetre continuum emission, observed at an angular resolution
of 20 milliarcsec (corresponding to 70 AU), reveals a bright compact central
component whose spectral index indicates that it composed of amorphous carbon
dust. Based on these findings, we conclude that this emission traces the
previously suggested dust disc observed in mid-infrared observations.
Therefore, our observations provide the first direct imaging of such a disc.
The H$^{12}$CN($J$=4$\rightarrow$3) line emission, observed at an angular
resolution of 300 milliarcsec (corresponding to 1000 AU), displays bipolar
structure with a north-south velocity gradient. From the position-velocity
diagram of this emission we identify the presence of an expanding disc and a
bipolar molecular outflow. The inclination of the disc is determined to be
$i$=72$^\circ$. The derived values for the de-projected expansion velocity and
the radius of the disc are $v_{\rm exp}$=53 km s$^{-1}$ and $R$=277 AU,
respectively. On the other hand, the de-projected expansion velocity of the
bipolar outflow detected in the H$^{12}$CN($J$=4$\rightarrow$3) emission of
approximately 1000 km s$^{-1}$. We propose that the molecular outflow has an
hourglass morphology with an opening angle of around 60$^{\circ}$. Our
observations unambiguously show that an equatorial disc and bipolar outflows
formed in Sakurai's object in less than 30 years after the born-again event
occurred, providing important constraints for future modelling efforts of this
phenomenon.
