  We revisit the abundances of neutron-capture elements in the metal-poor
([Fe/H]=-2.9) r-process-rich halo star CS 31082-001. Partly motivated by the
development of the new near-ultraviolet Cassegrain U-band Efficient
Spectrograph for the Very Large Telescope, we compiled an expanded line list
for heavy elements over the range 3000-4000 {\AA}, including hyperfine
structure for several elements. Combining archival near-ultraviolet spectra of
CS 31082-001 from the Hubble Space Telescope and the Very Large Telescope, we
investigate the abundances and nucleosynthesis of 35 heavy elements (Ge, Sr, Y,
Zr, Nb, Mo, Ru, Rh, Pd, Ag, Cd, Sn, Ba, La, Ce, Pr, Nd, Sm, Eu, Gd, Tb, Dy, Ho,
Er, Tm, Yb, Lu, Hf, Os, Ir, Pt, Pb, Bi, Th, and U). Our analysis includes the
first abundance estimates for tin, holmium, and ytterbium from these data, and
the first for lutetium from ground-based data, enabling a more complete view of
the abundance pattern of this important reference star. In general, the
r-process dominated elements are as enhanced as those in the Sun, particularly
for elements with Z $\ge$ 56 (Ba and heavier). However, the abundances for the
lighter elements in our sample, from Ge to Sn (31 $\le$ Z $\le$ 50), do not
scale with the solar abundance pattern. Moreover, the Ge abundance is deficient
relative to solar, indicating that it is dominantly an iron-peak rather than
neutron-capture element. Our results (or upper limits) on Sn, Pt, Au, Pb and Bi
all pose further questions, prompting further study on the origin and evolution
of the known r-rich and actinide-rich, metal-poor stars.
