Results from the test with the simulated PARSEC sample with high-resolution-like observational errors (see Sect. 2.2; e_Teff = 100 K, e_[Z/H] = 0.1 dex, e_log g = 0.1 dex, and e_mobs = 0.01 mag), using the full input parameter set (set 1: x = {[M/H] ,T_eff,log g,m,colours}). Left six panels: relative distance errors (observed – true) of the simulated stars shown as a function of the (true) main stellar model parameters T_eff, [M/H], log g, mass m_⋆, age τ, and distance d_true. The solid line marks the identity line, dashed lines indicate distance deviations of 20%. Upper right panel: relative distance error distribution in the T_eff− log g diagram. Lower right panel: relative distance uncertainty distribution in the T_eff− log g diagram. Clearly, distances to giant stars are much more prone to systematics and have larger uncertainties.