Summary of RV models and adopted priors.
|(2 planets + GP trained on y = K2 photometry)|
|Covariance amplitude, a [m s-1]|
|Exponential timescale, λ [days]||p(λ | y)|
|Coherence, Γ||p(Γ | y)|
|Periodic timescale, PGP [days]||p(PGP | y)|
|Additive jitter, s [m s-1]|
|γ0 [m s-1]|
|T0,b [BJD-2 450 000]|
|Kb [m s-1]|
|T0,c [BJD-2 450 000]|
|Kc [m s-1]|
|(2 planets + GP trained on y = BIS)|
|see Model 1|
|(2 planets + untrained GP)|
|see Model 1 with the|
|ln Exponential timescale, lnλ [days]|
|ln Coherence, lnΓ|
|ln Periodic timescale, lnPGP [days]|
|see Keplerian parameters in Model 1|
Notes. refers to a non-informative Jeffreys prior which is scale invariant; equal probability per decade which is necessary to sample multiple orders of magnitude (Gregory 2005). (◦) based on the transit light curve measurements from B17. (∗) m s-1 refers to a modified Jefferys prior on a parameter A which behaves like a uniform prior for A ≪ the knee at k m s-1 and behaves like a Jeffreys prior at A ≫ k up to l. We use a modified Jeffreys prior on the RV semi-amplitudes K to sample multiple decades as a Jeffreys prior but also include K = 0 m s-1 which a Jeffreys prior does not (Gregory 2005). (†) We further insist that e = h2 + k2 < 1.
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