Upper panel: the full line follows the loci of stellar masses that reproduce the observed atmospheric parameters (ADS solution) of HD 93840 with distance as independent parameter, the dashed and dashed-dotted lines follow the loci where stellar evolution models of Ekström et al. (2012) show the same T_eff as HD 93840, for the rotating and non-rotating case, respectively. Values along the curves indicate luminosities and flight times τ_flight to reach the distance, adopting the kinematic parameters from Table 1 and assuming ejection from the disk mid-plane, or evolutionary timescales τ_evol for the models to reach T_eff of HD 93840. The vertical short lines indicate the points where τ_evol  =  τ_flight. The vertical dotted line marks d_spec, as the division line where HD 93840 would switch from being overluminous to becoming underluminous. Lower panel: posterior cumulative distance distributions (CDF) derived from a Bayesian approach, using the Gaia EDR3 parallax after application of the zero-point correction of Maíz Apellániz (2022), and assuming an uncertainty inflated according to El-Badry et al. (2021, blue CDF), and when considering parallax bias according to Maíz Apellániz (2022, purple CDF). The grey horizontal lines represent the 16th, 50th, and 84th percentile.