  The latest analysis efforts in reverberation mapping are beginning to allow
reconstruction of echo images (or velocity-delay maps) that encode information
about the structure and kinematics of the broad line region (BLR) in active
galactic nuclei (AGNs). Such maps can constrain sophisticated physical models
for the BLR. The physical picture of the BLR is often theorized to be a
photoionized wind launched from the AGN accretion disk. Previously we showed
that the line-driven disk wind solution found in an earlier simulation by Proga
and Kallman is virialized over a large distance from the disk. This finding
implies that, according to this model, black hole masses can be reliably
estimated through reverberation mapping techniques. However, predictions of
echo images expected from line-driven disk winds are not available. Here, after
presenting the necessary radiative transfer methodology, we carry out the first
calculations of such predictions. We find that the echo images are quite
similar to other virialized BLR models such as randomly orbiting clouds and
thin Keplerian disks. We conduct a parameter survey exploring how echo images,
line profiles, and transfer functions depend on both the inclination angle and
the line opacity. We find that the line profiles are almost always single
peaked, while transfer functions tend to have tails extending to large time
delays. The outflow, despite being primarily equatorially directed, causes an
appreciable blue-shifted excess on both the echo image and line profile when
seen from lower inclinations ($i \lesssim 45^\circ$). This effect may be
observable in low ionization lines such as $\rm{H}\beta$.
