2013MNRAS.430.1473L

The timing errors for individual planetary transits using the photometric transit timing technique (TTVp) are derived for light curves contaminated with either white additive noise, realistic stellar noise or filtered stellar noise. For the case of white noise, the timing errors are derived analytically, while timing errors for realistic and filtered noise are numerically derived using solar data from the Solar and Heliospheric Observatory satellite. These results are then used to explore the conjecture that moons of transiting planets become easier to detect using the TTVp method the farther their planet is from the star. Using transit duration as a proxy for planet-star distance, it is found that in the case of realistic stellar noise, an increase in star-planet distance/transit duration does not necessarily lead to an increase in moon detectability.