Notes. The notation is as follows: 1 .. Ac1, 2 .. Ac2, 3 .. Aa1, 4 .. Aa2. The orbital elements are osculating for the epoch T₀ = 2453738.819100, where m₁ denotes the mass of body 1 (and so on for bodies 2, 3, 4); P₁ is the orbital period of the orbit (1+2), log e₁ logarithm of eccentricity, i₁ inclination, Ω₁ longitude of node, ϖ₁ longitude of pericentre, λ₁ true longitude (and so on for orbits (3+4), (1+2)+(3+4)); T₁ is the effective temperature of body 1, log g₁ logarithm of gravity, v_rot1 rotational velocity, γ systemic velocity, d_pc distance; n denotes the number of observations (RV, TTV, VIS, CLO, T3, SYN, SED, SKY2); χ² is simply unreduced χ². The nominal and alternative models use different weights (cf. ^(w)). Parameters flagged with ^(†)were derived from T, according to Harmanec (1988); those flagged with ^(f)were fixed. The angular orbital elements are expressed in the standard stellar reference frame; the (Ac1+Ac2) eclipsing binary is located in the centre.