  We study the sensitivity of future xenon- and argon-based dark matter and
neutrino detection experiments to low-energy atmospheric neutrinos. Not
accounting for experimental backgrounds, the primary obstacle for identifying
nuclear recoils induced by atmospheric neutrinos is the tail of the electron
recoil distribution due to $pp$ solar neutrinos. We use the NEST code to model
the solar and atmospheric neutrino signals in a xenon detector and find that an
exposure of 700 tonne-years will produce a $5\sigma$ detection of atmospheric
neutrinos. We explore the effect of different detector properties and find that
a sufficiently long electron lifetime is essential to the success of such a
measurement.
