TTVs are derived from Q1-Q17 Kepler data. x-axes: “Observed Tc” (Mid-Transit Time): EXOFAST’s best-fits from Normalized PDCSAP_FLUX Kepler light flux vs. time (BJD_tdb - 2454900) data. y-axes: “(O – C)”: difference between Observed Tc and the Calculated Tc from the graphically obtained linear ephemeris.
Figure 1.: KOI-2666.01, P = 64.04 days [Plot avg. error bars = ± 10.70 min. (smaller than symbols)] TTV_maximum: ~ 769.08 days, Amp_ttv_maximum: ~ 80.22 min. P_ttv: ~ 3933 days. Amp_ttv: ~ 769 minutes. Lomb-Scargle periodogram, candidate P_ttv: 1504.92 days; Power: 5.58; FAP: 0.00251. Linear ephemeris (this work): Tc = [64.03645654 ± 0.00231506](Tc#) + [92.02432083 ± 0.02869065]
Figure 3.: Added combination of Figures 1. and 2. [Plot error bars = ± 33.84 min.]
Numerous literature and major Tc#, Tc, and TTV tabulation references can be found on my "Summary" webpage following the table.
17 April 2015
Kepler KOI-2666 (KIC-5342061) 3-(or more?)-Planet System
Discussion: In the example of KOI-2666.01, after a partial (since much less than one cycle was observed by Kepler) sinusoidal curve-fit of the (O-C) vs. Time data showed (Figure 1. below) a periodicity (P_ttv) of ~ 3933 days (1504 days was observed in the Lomb-Scargle Periodogram (LSP) of the same data), a plot (Figure 2.) of the Residuals gave a good sinusoidal curve-fit with a periodicity of 424.74 ± 14.13 days (LSP: 421.41 days). The added combination of these two sinusoidal curves, arrayed in Figure 3., shows a complex overall curvature reasonably consistent with the initial data. While it is certainly possible (see recent work of Lithwick and others) that some of this unusual curvature obtains from eccentric orbits (and maybe even precessing eccentric orbits) of planetary objects in this system, it is also possible that at least 3 planets (with only KOI-2666.01 transiting) in near-circular orbits are mutually-interacting to give the TTV distribution observed.