Bern EXoplanet cooling curves (BEX) for planet masses m_p = 0.5–20 mM_⊙ (bottomto top) with different atmospheric boundary conditions (Eddington; Baraffe et al. 2003; Burrows et al. 1997; see legend). The Bern evolution (cooling) code completo 21 is used and compares very well to the original models. Units of milli-solar masses (1 mM_⊙ = 1.05 M_J) are usedto reproduce as closely as possible the tracks of Burrows et al. (1997) and Baraffe et al. (2003). The starting luminosities of the original AMES-COND (Baraffe et al. 2003) tracks are apparently not quite the same as for Burrows et al. (1997). The faint grey cross shows β Pic b (Bonnefoy et al. 2014b) as an example error bar.