Table 2.
Best-fit statistical properties of the models fitted to the dataset of this paper.
| Model | Npar | χ2 | Rχ2 | ΔAIC | ΔBIC |
|---|---|---|---|---|---|
| Planet | 32 | +2.4 | +0.0003 | +4.4 | +12 |
| Kepler | 30 | +4.0 | 0.0002 | +2.0 | –5.4 |
| PL2/Kepl1 | 30 | +19 | +0.0014 | +17 | +9.6 |
| PL3 | 31 | 15511.9 | 1.2466 | 15573.9 | 15804.3 |
| PL4 | 32 | +4.8 | +0.0005 | +6.8 | +14 |
| PL5 | 33 | –5.4 | –0.0002 | –1.4 | +14 |
| PL3DM10 | 39 | –17 | –0.0006 | –1.3 | +58 |
Notes. Npar is the number of parameters of the model, χ2 the minimum chi squared, Rχ2 is equal to χ2/Nd.o.f where Nd.o.f = 12474 − Npar. AIC and BIC are the Akaike and Bayesian information criteria, respectively. The ‘PL3’ line is the reference fit subtracted from all the other lines. All models assume GR. Models are described in Sect. 4.1: ‘Planet’ is the full 4-body numerical model; ‘Kepler’ is the purely Keplerian model without mutual interactions; ‘PLn’ are models with n sinusoidal harmonics following Eq. (1) in order to account for red noise; PL2 is equivalent to a planet in Keplerian orbit with the centre of mass of the triple system at leading order in eccentricity (no mutual interactions) and thus denoted ‘PL2/Kepl1’; PL3DM10 fits separate DM within ten evenly distributed intervals on top of three harmonics (We note the other models have DM and DM’ parameters, which have been removed here).
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