  Using Non-Redundant Mask interferometry (NRM), we searched for binary
companions to objects previously classified as Transitional Disks (TD). These
objects are thought to be an evolutionary stage between an optically thick disk
and optically thin disk. We investigate the presence of a stellar companion as
a possible mechanism of material depletion in the inner region of these disks,
which would rule out an ongoing planetary formation process in distances
comparable to the binary separation. For our detection limits, we implement a
new method of completeness correction using a combination of randomly sampled
binary orbits and Bayesian inference. The selected sample of 24 TDs belong to
the nearby and young star forming regions: Ophiuchus ($\sim$ 130 pc),
Taurus-Auriga ($\sim$ 140 pc) and IC348 ( $\sim$ 220 pc). These regions are
suitable to resolve faint stellar companions with moderate to high confidence
levels at distances as low as 2 au from the central star. With a total of 31
objects, including 11 known TDs and circumbinary disks from the literature, we
have found that a fraction of 0.38 $\pm$ 0.09 of the SEDs of these objects are
likely due to the tidal interaction between a close binary and its disk, while
the remaining SEDs are likely the result of other internal processes such as
photoevaporation, grain growth, planet disk interactions. In addition, we
detected four companions orbiting outside the area of the truncation radii and
we propose that the IR excesses of these systems are due to a disk orbiting a
secondary companion
