Surface density rendered plots of the HD 142527 protoplanetary disc. Each panel shows a different simulation at the same moment in time, but with different disc and binary parameters. The left panel reproduces the results of the R2 orbit in Price et al. (2018a) where the companion was shown to be responsible for the observed disc features: a large cavity, prominent spiral arms, and a misaligned inner disc. The middle panel uses the same disc parameters as the left panel, but uses the updated binary parameters in Table 3. The right panel is set up with the second solution of the updated binary parameters, and a smaller inner disc boundary to match the ratio of R_in/R_apoapsis of the simulation in the left panel. In the middle and right panels we find that, due to the close configuration of the updated binary orbit, the companion cannot be solely responsible for the observed disc features.