Velocity offset between Lyα and [CII] (filled circles) and between ISM and [CII] (empty circles) as a function of EW₀(Lyα) (top left panel), f_esc(Lyα) (top central panel), absolute magnitude in the far-UV M_FUV (top right panel), stellar mass (bottom left panel), SFR (bottom central panel), and E(B − V)_* (bottom right panel). The green (cyan) triangles show the running median of the Lyα (ISM) offset in bins of EW₀(Lyα), f_esc(Lyα), redshift, stellar mass, SFR, and E(B − V)_*. The error bars on the offset velocity mainly reflect the spectral resolution of the optical spectra: smaller error bars are for objects from DEIMOS, which have R ∼ 2000, while larger bars are in general from VIMOS/VUDS spectroscopy, which has a lower spectral resolution (R ∼ 230). The continuous lines are linear fits to the black points, and the p-value of the Spearman rank test (the probability of no correlation) is reported in each panel. In the first panel (Δv_Lyα vs. EW₀(Lyα) we show in red the correlation between the two quantities reported in Erb et al. (2014): the continuous line is our best fit to the data in their Fig. A.1, and the dashed lines contain 68% of their data points.