  Modeling the evolution of progenitors of gravitational-wave merger events in
binary stars faces two major uncertainties: the common-envelope phase and
supernova kicks. These two processes are critical for the final orbital
configuration of double compact-object systems with neutron stars and black
holes. Predictive one-dimensional models of common-envelope interaction are
lacking and multidimensional simulations are challenged by the vast range of
relevant spatial and temporal scales. Here, we present three-dimensional
hydrodynamic simulations of the common-envelope interaction of an initially
$10\,M_{\odot}$ red supergiant primary star with a black-hole and a
neutron-star companion. We show that the high-mass regime is accessible to full
ab-initio simulations. Nearly complete envelope ejection is reached assuming
that all recombination energy still available at the end of our simulation
continues to help unbinding the envelope. In contrast to previous assumptions,
we find that the dynamical plunge-in of both companions terminates at orbital
separations too wide for gravitational waves to merge the systems in a Hubble
time. We discuss the further evolution of the system based on analytical
estimates. A subsequent mass-transfer episode from the remaining $3\,M_{\odot}$
core of the supergiant to the compact companion does not shrink the orbit
sufficiently either. A neutron-star--neutron-star and neutron-star--black-hole
merger is still expected for a fraction of the systems if the supernova kick
aligns favorably with the orbital motion. For double neutron star
(neutron-star--black-hole) systems we estimate mergers in about $9 \%$ ($1 \%$)
of cases while about $77 \%$ ($94 \%$) of binaries are disrupted, i.e.,
supernova kicks actually enable gravitational-wave mergers in our cases;
however, we expect a reduction in predicted gravitational-wave merger events.
(abbr.)
