  We acquired and analyzed adaptive-optics imaging observations of asteroid (2)
Pallas from Keck II and the Very Large Telescope taken during four Pallas
oppositions between 2003 and 2007, with spatial resolution spanning 32-88 km
(image scales 13-20 km/pix). We improve our determination of the size, shape,
and pole by a novel method that combines our AO data with 51 visual
light-curves spanning 34 years of observations as well as occultation data.
  The shape model of Pallas derived here reproduces well both the projected
shape of Pallas on the sky and light-curve behavior at all the epochs
considered. We resolved the pole ambiguity and found the spin-vector
coordinates to be within 5 deg. of [long, lat] = [30 deg., -16 deg.] in the
ECJ2000.0 reference frame, indicating a high obliquity of ~84 deg., leading to
high seasonal contrast. The best triaxial-ellipsoid fit returns radii of a=275
km, b= 258 km, and c= 238 km. From the mass of Pallas determined by
gravitational perturbation on other minor bodies [(1.2 +/- 0.3) x 10-10 Solar
Masses], we derive a density of 3.4 +/- 0.9 g.cm-3 significantly different from
the density of C-type (1) Ceres of 2.2 +/- 0.1 g.cm-3. Considering the spectral
similarities of Pallas and Ceres at visible and near-infrared wavelengths, this
may point to fundamental differences in the interior composition or structure
of these two bodies.
  We define a planetocentric longitude system for Pallas, following IAU
guidelines. We also present the first albedo maps of Pallas covering ~80% of
the surface in K-band. These maps reveal features with diameters in the 70-180
km range and an albedo contrast of about 6% wrt the mean surface albedo.
