TTVs are derived from Q1-Q16 Kepler data.  x-axes: “Observed Tc” (Mid-Transit Time): EXOFAST’s best-fits from Kepler light flux vs. time data.  y-axes: “(O – C)”: difference between Observed Tc and the Calculated Tc from the graphically obtained linear ephemeris.  The plots are pictured in the order of orbital periods.

Planet candidate 410.01, according to its sinusoidal curve-fit, may indeed show a TTV but:(a) its amplitude, being highly unsymmetrical, is quite atypical: Amp_ttv_minimun appears to be -2.26 minutes, while its Amp_ttv_maximum, although not seen at all, is calculated to be +72.15 minute; and(b) its periodicity is quite large (7298.38 days) and much larger than was strongly indicated by its Lomb-Scargle periodogram: 1493.65 days, with a highly credible P-value of 0.0000.If there really is another planetary object perturbing 410.01, it seems likely that the curve-fitting, being limited to using data for part of just one very broad minimum, is at the root of these unusual characteristics.Alternatively, other effects (such as precession of an elliptical orbit, the presence of another star, etc.) may be operating to show the observed long trends.

KOI-410.01, P = 7.22 days
TTV_minimum: ~ 778.23 days, Amp_ttv_minimum: ~ -2.27 min.
[Predicted: 1st TTV_maximum: ~ 4427.42 days, Amp_ttv_maximum: ~ 72.15 min.]
[Predicted: P_ttv: ~ 7298.38 days.]
Lomb-Scargle periodogram, candidate P_ttv: 1493.65 days; Power: 39.84; P-value: 0.0000.
Linear ephemeris (this work): Tc = 7.21694998(Tc#) + 109.28362456

• For Q1-Q6 TTV data of 410.01 (thru ~ 563 (BJD-2454900, before the long-term curvature was clear) see: Ford2012arXiv-1201.1892.

22 Aug 2013
Kepler KOI-410 (KIC-5449777) 1-(or 2)-Planet System

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