Table 5.
Priors used in the analysis of VFTS 243.
| Parameter | Prior |
|---|---|
| log(m1,i/M⊙) | U(0.1, 3) |
| log(m2,i/M⊙) | U(0.1, 3) |
| log(Pi/d) | U(−1, 3) |
| ei | δ(ei) a |
| cos ii | U(0, 1) |
| ωi [rad] | U(0, 2π) |
| Ωi [rad] | U(0, 2π) |
| vk [km s−1] | U(0, 400) |
| fΔM | U(0, 1) |
| cos θ | U(−1, 1) |
| ϕ [rad] | U(0, 2π) |
| νi [rad] | U(0, 2π) b |
| Vα, env [km s−1] | 𝒩(393, 42) (1) |
| Vδ, env [km s−1] | 𝒩(146, 40) (1) |
| Vr, env [km s−1] | 𝒩(270, 11) (2) |
Notes. These are the default distributions used in all variations, except where noted. They are chosen to be wide and uninformative.
The circular orbit prior is replaced with the eccentric prior U(0, 1) in the final model variation.
The true anomaly prior is sampled uniformly for simplicity, then later reweighted so that νi is more correctly uniform in time.
References: (1) Gaia Collaboration (2023); (2) Almeida et al. (2017).
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