2023MNRAS.520.5002K

We map the 3D kinematics of the Galactic disc out to 3.5 kpc from the Sun, and within 0.75 kpc from the mid-plane of the Galaxy. To this end, we combine high-quality astrometry from Gaia EDR3, with heliocentric line-of-sight velocities from Gaia DR2, and spectroscopic surveys including APOGEE, GALAH, and LAMOST. We construct an axisymmetric model for the mean velocity field, and subtract this on a star-by-star basis to obtain the residual velocity field in the Galactocentric components (V_ϕ, V_R, V_z), and V_los. The velocity residuals are quantified using the power spectrum, and we find that the peak power (A/[km s^–1]) in the mid-plane (|z| < 0.25 kpc) is (A_ϕ, A_R, A_Z, A_los) = (4.2,8.5,2.6,4.6), at 0.25 < |z|/[kpc] < 0.5, is (A_ϕ, A_R, A_Z, A_los) = (4.0,7.9,3.6,5.3), and at 0.5 < |z|/[kpc] < 0.75, is (A_ϕ, A_R, A_Z, A_los) = (1.9,6.9,5.2,6.4). Our results provide a sophisticated measurement of the streaming motion in the disc and in the individual components. We find that streaming is most significant in V_R, and at all heights (|Z|) probed, but is also non-negligible in other components. Additionally, we find that patterns in velocity field overlap spatially with models for spiral arms in the Galaxy. Our simulations show that phase-mixing of disrupting spiral arms can generate such residuals in the velocity field, where the radial component is dominant, just as in real data. We also find that with time evolution, both the amplitude and physical scale of the residual motion decrease.