  We present a high-resolution (R~35,000), high signal-to-noise (S/N>200)
Magellan/MIKE spectrum of the star RAVE J094921.8-161722, a bright (V=11.3)
metal-poor red giant star with [Fe/H] = -2.2, identified as a carbon-enhanced
metal-poor (CEMP) star from the RAVE survey. We report its detailed chemical
abundance signature of light fusion elements and heavy neutron-capture
elements. We find J0949-1617 to be a CEMP star with s-process enhancement that
must have formed from gas enriched by a prior r-process event. Light
neutron-capture elements follow a low-metallicity s-process pattern, while the
heavier neutron-capture elements above Eu follow an r-process pattern. The Pb
abundance is high, in line with an s-process origin. Thorium is also detected,
as expected from an r-process origin, as Th is not produced in the s-process.
We employ nucleosynthesis model predictions that take an initial r-process
enhancement into account, and then determine the mass transfer of carbon and
s-process material from a putative more massive companion onto the observed
star. The resulting abundances agree well with the observed pattern. We
conclude that J0949-1617 is the first bonafide CEMP-r+s star identified. This
class of objects has previously been suggested to explain stars with
neutron-capture element patterns that originate from neither the r- or
s-process alone. We speculate that J0949-1617 formed in an environment similar
to those of ultra-faint dwarf galaxies like Tucana III and Reticulum II, which
were enriched in r-process elements by one or multiple neutron star mergers at
the earliest times.a
