  Turbulence is thought to play a role in the heating of the solar wind plasma,
though many questions remain to be solved regarding the exact nature of the
mechanisms driving this process in the heliosphere. In particular, the physics
of the collisionless interactions between particles and turbulent
electromagnetic fields in the kinetic dissipation range of the turbulent
cascade remains incompletely understood. A recent analysis of an interval of
Magnetosphere Multiscale (MMS) observations has used the field-particle
correlation technique to demonstrate that electron Landau damping is involved
in the dissipation of turbulence in the Earth's magnetosheath. Motivated by
this discovery, we perform a high-resolution gyrokinetic numerical simulation
of the turbulence in the MMS interval to investigate the role of electron
Landau damping in the dissipation of turbulent energy. We employ the
field-particle correlation technique on our simulation data, compare our
results to the known velocity-space signatures of Landau damping outside the
dissipation range, and evaluate the net electron energization. We find
qualitative agreement between the numerical and observational results for some
key aspects of the energization and speculate on the nature of disagreements in
light of experimental factors, such as differences in resolution, and of
developing insights into the nature of field-particle interactions in the
presence of dispersive kinetic Alfv\'en waves.

Plasma Physics