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The astrometric sample of Gaia allows us to study the outermost Galacticdisc, the halo and their interface. It is precisely at the very edge of thedisc where the effects of external perturbations are expected to be the mostnoticeable. Our goal is to detect the kinematic substructure present in thehalo and at the edge of the Milky Way (MW) disc, and provide observationalconstraints on their phase-space distribution. We download, one HEALpix at atime, the proper motion histogram of distant stars, to which we apply a WaveletTransformation to reveal the significant overdensities. We then analyse thelarge coherent structures that appear in the sky. We reveal a sharp yet complexanticentre dominated by Monoceros (MNC) and the Anticentre Stream (ACS) in thenorth, which we find with an intensity comparable to the Magellanic clouds andthe Sagittarius stream, and by MNC south and TriAnd at negative latitudes. Ourmethod allows us to perform a morphological analysis of MNC and ACS, bothspanning more than 100$^\circ$ in longitude, and to provide a high puritysample of giants with which we track MNC down to latitudes as low as$\sim$5$^\circ$. Their colour-magnitude diagram is consistent with extendedstructures at a distance of $\sim$10-11 kpc originated in the disc, with a verylow ratio of RR Lyrae over M giants, and kinematics compatible with therotation curve at those distances or only slightly slower. We present a precisecharacterisation of MNC and ACS, two previously known structures that ourmethod reveals naturally, allowing us to detect them without limiting ourselvesto a particular stellar type and, for the first time, using only kinematics.Our results allow future studies to model their chemo-dynamics and evolution,thus constraining some of the most influential processes that shaped the MW.

The outer disc in shambles: blind detection of Monoceros and ACS with Gaia's astrometric sample