Left: pebble accretion efficiency ϵ and the Stokes number for different values of the vertical turbulence strength α_turb. The figure uses the planet-to-star mass ratio of 3 × 10⁻⁷ (i.e. ~ 0.1 M_E for a Sun-like star), the gas disc aspect ratio of h_g = 0.03, and the disc radial pressure gradient of η = 1.0 × 10⁻³ as in Fig. 4 of Ormel & Liu (2018). Circles show ϵ from Ormel & Liu (2018) and crosses show corresponding ϵ from Ida et al. (2016). Right: pebble isolation masses estimated by Ataiee et al. (2018; orange) and Bitsch et al. (2018; green), compared with our default case from Ida et al. (2016; blue). Also plotted are the critical migration transition masses (Eq. (10), red).