  Almost all meteorite impacts occur at oblique incidence angles, but the
effect of impact angle on crater size is not well understood, especially for
large craters. To improve oblique impact crater scaling, we present a suite of
simulations of complex crater formation on Earth and the Moon over a range of
impact angles, velocities and impactor sizes. We show that crater diameter is
larger than predicted by existing scaling relationships for oblique impacts and
for impacts steeper than 45$^{\circ}$ shows little dependence on obliquity.
Crater depth, volume and diameter depend on impact angle in different ways such
that relatively shallower craters are formed by more oblique impacts. Our
simulation results have implications for how crater populations are determined
from impactor populations and vice-versa. Our results suggest that existing
approaches to account for impact obliquity may underestimate the number of
craters larger than a given size by as much as 40%.
