  The Carminati and McLenaghan (CM) curvature invariants are powerful tools for
probing spacetimes. Henry et al. formulated a method of plotting the CM
curvature invariants to study black holes. The CM curvature invariants are
scalar functions of the underlying spacetime. Consequently, they are
independent of the chosen coordinates and characterize the spacetime. For Class
B1 spacetimes, there are four independent CM curvature invariants: R, r1, r2,
and w2. Lorentzian traversable wormholes and warp drives are two theoretical
solutions to Einstein's field equations, which allow faster-than-light (FTL)
transport. The CM curvature invariants are plotted and analyzed for these
specific FTL spacetimes: (i) the Thin-Shell Flat-Face wormhole, (ii) the
Morris-Thorne wormhole, (iii) the Thin-Shell Schwarzschild wormhole, (iv) the
exponential metric, (v) the Alcubierre metric at constant velocity, (vi) the
Nat\'ario metric at constant velocity, and (vii) the Nat\'ario metric at an
accelerating velocity. Plots of the wormhole CM invariants confirm their
traversability and show how to distinguish the wormholes. The warp drive CM
invariants reveal key features such as a flat harbor in the center of each warp
bubble, a dynamic wake for each warp bubble, and rich internal structure(s) of
each warp bubble.
