  Extremely metal poor stars have been the focus of much recent attention owing
to the expectation that their chemical abundances can shed light on the metal
and dust yields of the earliest supernovae. We present our most realistic
simulation to date of the astrophysical pathway to the first metal enriched
stars. We simulate the radiative and supernova hydrodynamic feedback of a
$60\,M_\odot$ Population III star starting from cosmological initial conditions
realizing Gaussian density fluctuations. We follow the gravitational
hydrodynamics of the supernova remnant at high spatial resolution through its
freely-expanding, adiabatic, and radiative phases, until gas, now
metal-enriched, has resumed runaway gravitational collapse. Our findings are
surprising: while the Population III progenitor exploded with a low energy of
$10^{51}\,\text{erg}$ and injected an ample metal mass of $6\,M_\odot$, the
first cloud to collapse after the supernova explosion is a dense surviving
primordial cloud on which the supernova blastwave deposited metals only
superficially, in a thin, unresolved layer. The first metal-enriched stars can
form at a very low metallicity, of only $2-5\times10^{-4}\,Z_\odot$, and can
inherit the parent cloud's highly elliptical, radially extended orbit in the
dark matter gravitational potential.
