  We have mapped the number density and mean vertical velocity of the Milky
Way's stellar disk out to roughly two kiloparsecs from the Sun using Gaia Data
Release 3 (DR3) and complementary photo-astrometric distance information from
StarHorse. For the number counts, we carefully masked spatial regions that are
compromised by open clusters, great distances, or dust extinction and used
Gaussian processes to arrive at a smooth, non-parametric estimate for the
underlying number density field. We find that the number density and velocity
fields depart significantly from an axisymmetric and mirror-symmetric model.
These departures, which include projections of the Gaia phase-space spiral,
signal the presence of local disturbances in the disk. We identify two features
that are present in both stellar number density and mean vertical velocity. One
of these features appears to be associated with the Local Spiral Arm. It is
most prominent at small heights and is largely symmetric across the mid-plane
of the disk. The density and velocity field perturbations are phase-shifted by
roughly a quarter wavelength, suggesting a breathing mode that is propagating
in the direction of Galactic longitude $l\sim 270$ deg. The second feature is a
gradient in the stellar number density and mean vertical velocity with respect
to Galactocentric radius. This feature, which extends across the entire region
of our analysis, may be associated with the extension of the Galactic warp into
the Solar neighbourhood in combination with more localised bending waves.
