  We identify the maximum cross sections probed by single-scatter ``WIMP"
searches in dark matter direct detection. Due to Poisson fluctuations in
scatter multiplicity, these ceilings scale logarithmically with mass for heavy
dark matter and often lie in regions probed by multiscatter searches. Using a
generalized formula for single-scatter event rates we recast WIMP searches by
the quintal-to-tonne scale detectors XENON1T, XENONnT, LZ, PANDAX-II,
PANDAX-4T, DarkSide-50 and DEAP-3600 to obtain ceilings and floors up to a few
$10^{17}$ GeV mass and $10^{-22}$ cm$^2$ per-nucleus cross section. We do this
for coherent, geometric, isospin-violating xenophobic and argophobic
spin-independent scattering, and neutron-only and proton-only spin-dependent
scattering. Future large-exposure detectors would register an almost
irreducible background of atmospheric neutrinos that would determine a dark
matter sensitivity ceiling that we call the ``neutrino roof", in analogy with
the well-studied ``neutrino floor". Accounting for this background, we estimate
the reaches of the 10$-$100 tonne scale DarkSide-20k, DARWIN/XLZD, PANDAX-xT,
and Argo, which would probe many decades of unconstrained parameter space up to
the Planck mass, as well as of $10^3-10^4$ tonne scale noble liquid detectors
that have been proposed in synergy with neutrino experiments.
