  We present photodynamical models of four eclipsing binary systems that are
members of higher-order multiple systems. We provide some radial velocities
measurements and use recent TESS data for three of the systems. KIC 7668648
consists of an eclipsing binary (P=27.8 d) with late-type stars that has a
low-mass star on a roughly coplanar outer orbit (P=208 d). There are eclipse
events involving the third star that allow for the precise determination of the
system parameters. KIC 10319590 consists of a binary (P=21.3 d) with late-type
stars that stopped eclipsing about a third of the way into the Kepler mission.
We show that the third star in this system is a Sun-like star on an inclined
outer orbit (P=456 d). We present the first comprehensive solution for KIC
5255552 and demonstrate that it is a 2 + 2 system consisting of an eclipsing
binary (P_1 = 32.5 d) with late-type stars paired with a non-eclipsing binary
(P_2 = 33.7 d) with lower-mass stars. The two binaries have nearly coplanar
orbits and a roughly aligned outer orbit (P=878 d). There are extra eclipses
involving the component stars of the non-eclipsing binary, which leads to
relatively small uncertainties in the system parameters. EPIC 220204960
consists of a pair of eclipsing binaries that both consist of two low-mass
stars with a poorly determined outer orbit. Because of the relatively short
time span of the observations, the masses and radii of the component stars can
only be determined with accuracies of ~10% and ~5%, respectively. We show that
the most likely period of the outer orbit is 957 days, with a 1-sigma range of
595 to 1674 days. We can only place weak constraints on the mutual inclinations
of the orbital planes, and additional radial velocity measurements and/or
additional eclipse observations would allow for much tighter constraints on the
properties of the outer orbit.
