Sensitivity curves for an illustrative binary TOI in our sample in which it is currently unknown which of the binary stars is the host of the transiting exoplanet TOI 3353.01. In both panels, the “x” indicates the orbital period and corrected radius of the planet. An Earth-sized planet orbiting the primary or a giant planet orbiting the secondary would result in transits with the same SNR. The SNR = 9 contour is the TESS detection threshold for transits by TOIs that were detected via the QLP pipeline, as TOI 3353.01 was. While TESS would be expected to detect Earth-sized short-period exoplanets transiting the primary, it would be sensitive only to planets with ≳4 R_⊕ if they transit the secondary.