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KOI's (Blue)  or
K2 Objects (Green)

TTVs are derived from Q0-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: KOI-1476.01, P = 56.36 days [Plot avg. error bars = ± 5.99 min.]
The following are obtained from considerably less than one full cycle of periodicity:
TTV_maximum: 827.92 ± 1002.06 days, Amp_ttv_maximum: 31.12 ± 166.34 min.
P_ttv: 2819.26 ± 2413.31 days.
Amp_ttv: 165.46 ± 235.23 minutes.
Lomb-Scargle periodogram, periodicity (P_ttv): 1500.41 days; Power: 8.72; FAP: 6.134 x 10^-7.
Linear ephemeris (this work): Tc = 56.35903247(Tc#) + 155.31743043

Literature Tc#, Tc, and TTV Major Tabulations and Other References:
• For Q0-6 TTV data (thru ~ 563 (BJD-2454900) days): Ford et al., 2012, arXiv-1201.1892.
• For Q0-10 TTV data (thru ~ 934 (BJD-2454900) days): Rowe et al., 2014, arXiv-1402.6534.
• For Q0-12 TTV data (thru ~ 1116 (BJD-2454900) days): Mazeh et al., 2013, arXiv-1301.5499.
• For Q0-12 Calc. properties from TTVs: Hadden & Lithwick, 2013, arXiv-1310.7942.
• For Q0-13/14 TTV data, Xie:
• Two ground-based Kepler-TTV-follow-up programs are in place at the moment: --- Gary, "KAFO" project: --- von Essen, "KOINet":

12 May 2014
Kepler KOI-1476 (KIC-12406749) 2-(or more?)-Planet System

TTV Evidence:
The presence of both a credible (i.e.: False Alarm Probability (FAP) < 0.1) periodicity in the Lomb-Scargle Periodogram (LSP) of [(O-C) vs. Time] ("TTVxy") data points, along with a sinusoidal distribution of the same points displaying a corresponding periodicity ("P_ttv") (see Figure(s) below), is strongly suggestive of the presence of an unseen (non-transiting), gravitationally perturbing planetary object(s) in the system.

When periodicity values from both methods are large…and visually obvious in the [(O-C) vs. Time] plot)…, they may not correspond very closely if considerably less than one cycle of periodicity has been observed.  This condition would significantly affect both the choice of "best-fit" sinusoidal curve and the precision of the LSP periodicity.  This is apparently true for KOI-1476.01.