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TTV-not-so-fast: Uniqueness and Degeneracy in Perturbing Planet Parameters

  • Authors: Caleb Lammers, Joshua N. Winn

Caleb Lammers and Joshua N. Winn 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 9.

KOI-134. Top panel: χ2 vs. period ratio (Ndof  =  27). Many 1:N solutions provide a satisfactory fit to the data. Second panel: TTVs from E. Nabbie et al. (2025). The gray curve is a GP model, used as a smooth interpolant to separate long- and short-timescale variations. Third panel: high-pass-filtered TTVs obtained by subtracting the GP. The red curve shows the best variant of the 1:2 solution (E. Nabbie et al. 2025), and the blue curve shows the 1:3 solution. Fourth panel: residuals of the 1:2 solution (rms  =  1.2 minutes) and the 1:3 solution (rms  =  1.1 minutes). Fifth panel: TDVs and predictions of the 1:2 and 1:3 models. Both models fit the data well; KOI-134’s TTV solution is not unique, and does not necessarily involve a companion with a large mutual inclination.

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