  Plasma turbulence plays a critical role in the transport of energy from
large-scale magnetic fields and plasma flows to small scales, where the
dissipated turbulent energy ultimately leads to heating of the plasma species.
A major goal of the broader heliophysics community is to identify the physical
mechanisms responsible for the dissipation of the turbulence and to quantify
the consequent rate of plasma heating. One of the mechanisms proposed to damp
turbulent fluctuations in weakly collisional space and astrophysical plasmas is
electron Landau damping. The velocity-space signature of electron energization
by Landau damping can be identified using the recently developed field-particle
correlation technique. Here, we perform a suite of gyrokinetic turbulence
simulations with ion plasma beta values of 0.01, 0.1, 1, and 10 and use the
field-particle correlation technique to characterize the features of the
velocity-space signatures of electron Landau damping in turbulent plasma
conditions consistent with those observed in the solar wind and planetary
magnetospheres. We identify the key features of the velocity-space signatures
of electron Landau damping as a function of varying plasma \beta_i to provide a
critical framework for interpreting the results of field-particle correlation
analysis of in situ spacecraft observations of plasma turbulence.
