  Five self-lensing binaries (SLBs) have been discovered with data from the
\textit{Kepler} mission. One of these systems is KIC 8145411, which was
reported to host an extremely low mass (ELM; $0.2\,M_{\odot}$) white dwarf (WD)
in a 456-day orbit with a solar-type companion. The system has been dubbed
"impossible", because evolutionary models predict that $\sim 0.2\,M_{\odot}$
WDs should only be found in tight orbits ($P_{\rm orb} \lesssim$ days). In this
work, we show that KIC 8145411 is in fact a hierarchical triple system: it
contains a WD orbiting a solar-type star, with another solar-type star $\sim
700\,$AU away. The wide companion was unresolved in the Kepler light curves,
was just barely resolved in Gaia DR3, and is resolved beyond any doubt by
high-resolution imaging. We show that the presence of this tertiary confounded
previous mass measurements of the WD for two reason: it dilutes the amplitude
of the self-lensing pulses, and it reduces the apparent radial velocity (RV)
variability amplitude of the WD's companion due to line blending. By jointly
fitting the system's light curves, RVs, and multi-band photometry using a model
with two luminous stars, we obtain a revised WD mass of $(0.53 \pm
0.01)\,M_{\odot}$. Both luminous stars are near the end of their main-sequence
evolution. The WD is thus not an ELM WD, and the system does not suffer the
previously proposed challenges to its formation history. Similar to the other
SLBs and the population of astrometric WD binaries recently identified from
Gaia data, KIC 8145411 has parameters in tension with standard expectations for
formation through both stable and unstable mass transfer. The system's
properties are likely best understood as a result of unstable mass transfer
from an AGB star donor.
