Top: same as Fig. 3, except that a possible transit of HD 10180 b was included in the global model. Highest posterior probability transit model for HD 10180 b is shown in purple. The posterior PDF for the transit timing of HD 10180 b derived from an RV analysis assuming 7 planets is shown above the figure. Bottom: 2013 Warm Spitzer photometry for HD 10180 binned per 30 min, corrected for the instrumental effects, normalized, and folded on the transit ephemeris for HD 10180 b based on our tentative detection of a transit and on the results of an RV analysis assuming 7 planets (dT = time from most likely mid-transit time).