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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 4.

KOI-884. Top panel: χ2 vs. period ratio (Ndof  =  95). The 3:2 solution provides the best fit, followed closely by the 3:1 and 3:5 solutions. Second panel: TTVs from D. Nesvorný et al. (2014), along with a GP model that provides a smooth interpolation to separate long- and short-timescale variations. The χ2 value associated with the GP model is marked by a horizontal gray line in the top panel; many solutions can reproduce this smooth variation. Third panel: high-pass-filtered TTVs obtained by subtracting the GP. The red curve shows the best variant of the 3:1 solution (D. Nesvorný et al. 2013). The blue curve shows the 3:2 solution, which provides a somewhat superior fit. Fourth panel: residuals of the 3:2 solution (rms  =  4.0 minutes) and the 3:1 solution (rms  =  6.0 minutes) Fifth panel: TDVs and predictions of the 3:2 and 3:1 models. KOI-884b’s TTV solution is at least borderline unique, but the best solution has not been reported in the literature.

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