Upper panels: bisector span measurements of WASP-65 (left) and WASP-75 (right) as a function of radial velocity. The horizontal dotted line marks the mean line bisector span ⟨ V_span ⟩  =  −0.017 km s^-1, and ⟨ V_span ⟩  = 0.013 km s^-1, respectively. Lower panels: bisector span measurements as a function of time (BJD_UTC – 2 450 000.0) for WASP-65 (left) and WASP-75 (right). The bisector spans of both planet hosts are of the same order of magnitude as the errors in the radial velocity measurements, and show no significant variation nor correlation with radial velocity or time. This suggests that the radial velocity variations (with semi-amplitudes of K₁ = 0.249    ±    0.005 km s^-1 for WASP-65b, and K₁ = 0.146    ±    0.004 km s^-1 for WASP-75b) are due to Doppler shifts of the stellar lines induced by a planetary companion rather than stellar profile variations due to stellar activity or a blended eclipsing binary.