Sub-Jupiter gas giants orbiting giant stars uncovered using a Bayesian framework

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Volume 704 (December 2025)

A&A, 704 (2025) A283

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Table F.6

HIP 111909 posterior probability (p (θ|D, M) maxima for the best-fit models for each of the examined model scenarios.

Tightly Constrained Eccentricity
e_TC Model	WNO	BLCO	BSLCO	MAO	BLCMA	BSLCMA
	473.2 (k2)	473.1 (k2)	479.0 (k2)	489.4 (k2)	493.3 (k2)	497.1 (k2)

Constrained Eccentricity
e_C Model	WNO	BLCO	BSLCO	MAO	BLCMA	BSLCMA
	469.2 (k2)	472.7 (k2)	477.4 (k2)	485.3 (k2)	490.1 (k2)	490.8 (k2)

Fixed Eccentricity
e_F Model	WNO	BLCO	BSLCO	MAO	BLCMA	BSLCMA
	457.6 (k2)	461.5 (k2)	465.6 (k2)	473.0 (k2)	478.3 (k2)	481.0 (k2)

The values in brackets represent the model that the maximum posterior probability was drawn from.

The values in square brackets represent the best preferred model fit, although the signal was not confirmed in other model sets.

WNO: Model that includes white noise only.

BLCO: BIS linear correlation terms.

BSLCO: Combined BIS and S-index linear correlation terms.

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