  We outline a photometric method for detecting the presence of a
non-transiting short-period giant planet in a planetary system harboring one or
more longer period transiting planets. Within a prospective system of the type
that we consider, a hot Jupiter on an interior orbit inclined to the
line-of-sight signals its presence through approximately sinusoidal full-phase
photometric variations in the stellar light curve, correlated with
astrometrically induced transit timing variations for exterior transiting
planets. Systems containing a hot Jupiter along with a low-mass outer planet or
planets on inclined orbits are a predicted hallmark of in situ accretion for
hot Jupiters, and their presence can thus be used to test planetary formation
theories. We outline the prospects for detecting non-transiting hot Jupiters
using photometric data from typical \textit{Kepler} objects of interest (KOIs).
As a demonstration of the technique, we perform a brief assessment of
\textit{Kepler} candidates and identify a potential non-transiting hot Jupiter
in the KOI-1822 system. Candidate non-transiting hot Jupiters can be readily
confirmed with a small number of Doppler velocity observations, even for stars
with $V\gtrsim14$.
