  Using TESS 20-sec cadence data, we have discovered an unusual combination of
pulsating stars in what we infer to be a binary system. The binary consists of
a standard $\delta$ Scuti star with pulsations over the range 32-41 d$^{-1}$;
this is in a likely wide orbit with a hot subdwarf B (sdB) star, which itself
has a large-amplitude p-mode pulsation at 524 d$^{-1}$. We establish
constraints on the period of the putative binary by using radial velocity
measurements of the $\delta$~Scuti star and show that any sdB companion star
must orbit with a period greater than a few tens of days. Our identification of
this sdB binary serves as an important addition to the relatively small number
of sdB binaries known to have orbital periods longer than a few days. We model
such a binary using {\tt MESA} and find that this system could be formed
through stable, nonconservative mass transfer from either a low- or
intermediate-mass progenitor, without undergoing a common envelope phase.
