Scroll Down  to

KOI's (Blue)  or
K2 Objects (Green)

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.

Discussion:Distinct curvature is seen in the [(O-C) vs. Tc] plot of KOI_350.01.  The magnitude of the P_ttv from the best sinusoidal fit and the Lomb-Scargle periodogram do not agree.  This is not surprising in such as case where only a small portion of the (sinusoidal) periodicity is available.  So while it is possible that another planetary object is causing the observed TTV, it is also possible that another effect, such as orbital precession of an eccentric orbit, is responsible.

KOI-350.01, P = 12.99 days [Plot error bars = ± 5.17 min.]
TTV_maximum: ~ 704 days, Amp_ttv_maximum: ~ 20 min.
"P_ttv": ~ 4406 days.
Lomb-Scargle periodogram, candidate "P_ttv": 1525.55 days; Power: 13.18; P-value: 0.00141.
Linear ephemeris (this work): Tc = 12.99081425(Tc#) + 110.23673293

• For Q0-Q6 TTV data of 350.01 (thru ~ 563 (BJD-2454900) days), see: Ford et al., 2012, arXiv-1201.1892.
• For Q0-12 TTV data of 350.01 (thru ~ 1116 (BJD-2454900) days), see: Mazeh et al., 2013, arXiv-1301.5499.

7 Nov 2013
Kepler KOI-350.01 (KIC-11395587) 2-(or more?)-Planet System