  One of the simplest ways to identify an exoplanetary transit is to phase fold
a photometric time series upon a trial period - leading to a coherent stack
when using the correct value. Such phase-folded transits have become a standard
data visualisation in modern transit discovery papers. There is no analogous
folding mechanism for exomoons, which would have to represent some kind of
double-fold; once for the planet and then another for the moon. Folding with
the planet term only, a moon imparts a small decrease in the surrounding
out-of-transit averaged intensity, but its incoherent nature makes it far less
convincing than the crisp stacks familiar to exoplanet hunters. Here, a new
approach is introduced that can be used to achieve the transit origami needed
to double fold an exomoon, in the case where a planet exhibits TTVs. This
double fold has just one unknown parameter, the satellite-to-planet mass ratio,
and thus a simple one-dimensional grid search can be used to rapidly identify
power associated with candidate exomoons. The technique is demonstrated on
simulated light curves, exploring the breakdown limits of close-in and/or
inclined satellites. As an example, the method is deployed on Kepler-973b, a
warm mini-Neptune exhibiting an 8 minute TTV, where the possibility that the
TTVs are caused by a single exomoon is broadly excluded, with upper limits
probing down to a Ganymede-sized moon.
