as the ratio of the observed TTV amplitude to the timing measurement uncertainty), one still needs at least about 15 transits, continuous or not, for the inverse problem to have a unique solution.

The [*Kepler*]{} mission, of course, changed that, but not being part of the [*Kepler*]{} team did not help. Thus, I became somewhat disheartened while watching the discoveries of Kepler-9b,c, which was the first planetary system characterized from TTVs (Holman et al. 2010), Kepler-19b, which was the first case that showed clear TTV evidence for an unseen planet (Ballard et al. 2011), and others. It looked as if the train departed leaving me behind. In the meanwhile, I improved the validity of the codes for strongly inclined systems and eccentric transiting planets, performed a tentative analysis of COROT-1b, TrES-1b and HD 189733b, and waited for something.

That something happened in November 2011 when I was on a sabbatical leave at the Nice observatory, in southern France. I received an unexpected email from David Kipping, then Carl Sagan Fellow at the Harvard-Smithsonian Center for Astrophysics. David invited me to be a member of a small team of researchers known as the [*Hunt for Exomoons with Kepler*]{} (HEK; Kipping et 