Amplitude of the obliquity oscillation for HD 40307 g as a function of initial obliquity and rotation period. Compare to Figure 8 in Brasser et al. (2014). The left panel started with ﹩\psi +{\rm{\Omega }}=0^\circ ﹩, the right with ﹩\psi +{\rm{\Omega }}=180^\circ ﹩. There is a secular resonance at rotation rates ﹩\lesssim 2﹩ days, similar to resonances for Kepler-62 f in Figure 5.