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Fig. A.4


Corner plot of the fitted parameters of the MCMC solutions using a Keplerian orbit (parameters P, K, e sin ω, e cos ω, Tper) and a GP noise term (hyper-parameters PQP, KQP, w, λ) to the RVs of HARPS-N S2 to S6 and CARMENES of Gl 49. The solutions included in this plot exceed the ln L value of a fit with a GP term only (see Table 4) plus the 1% FAP value that we calculate empirically in Sect. 4.2.

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