  We present the first wide-field near-infrared adaptive optics images of
Carina's Western Wall (G287.38-0.62), one of the brightest and most
well-defined irradiated interfaces known in a region of massive star formation.
The new narrowband H$_2$ 2.12$\mu$m, Br-$\gamma$ and K-continuum images trace
the photoevaporative flow from the cloud and identify locations where
UV-radiation from the surrounding massive stars excites molecular hydrogen to
fluoresce. With a field of view of $\sim$ 1.5' $\times$ 2.9' and spatial
resolution between 60 $-$ 110 mas, the new images show a spectacular level of
detail over a large area, and presage what JWST should achieve. The Wall is
convex in shape, with a large triangular-shaped extension near its apex. The
interface near the apex consists of 3 $-$ 4 regularly-spaced ridges with
projected spacings of $\sim$ 2000 AU, suggestive of a large-scale
dynamically-important magnetic field. The northern edge of the Wall breaks into
several swept-back fragments of width $\sim$ 1800 AU that resemble
Kelvin-Helmholtz instabilities, and the southern part of the Wall also shows
complex morphologies including a sinusoidal-like variation with a
half-wavelength of 2500 AU. Though the dissociation front must increase the
density along the surface of the Wall, it does not resolve into pillars that
point back to the ionization sources, as could occur if the front triggered new
stars to form. We discovered that MHO 1630, an H$_2$ outflow with no clear
driving source in the northern portion of the Wall, consists of a series of bow
shocks arrayed in a line.
