  Heliospheric plasma turbulence plays a key role in transferring the energy of
large-scale magnetic field and plasma flow fluctuations to smaller scales where
the energy can be dissipated, ultimately leading to plasma heating.
High-quality measurements of electromagnetic fields and electron velocity
distributions by the Magnetospheric Multiscale (MMS) mission in Earth's
magnetosheath present a unique opportunity to characterize plasma turbulence
and to determine the mechanisms responsible for its dissipation. We apply the
field-particle correlation technique to a set of twenty MMS magnetosheath
intervals to identify the dissipation mechanism and quantify the dissipation
rate. It is found that 95% of the intervals have velocity-space signatures of
electron Landau damping that are quantitatively consistent with linear kinetic
theory for the collisionless damping of kinetic Alfv\'en waves. About 75% of
the intervals contain asymmetric signatures, indicating a local imbalance of
kinetic Alfv\'en wave energy flux in one direction along the magnetic field
than the other. About one third of the intervals have an electron energization
rate with the same order-of-magnitude as the estimated turbulent cascade rate,
suggesting that electron Landau damping plays a significant, and sometimes
dominant, role in the dissipation of the turbulent energy in these
magnetosheath intervals.
