Schematic showing how we model planets across epochs with orbital motion. The solid black line shows the path of a hypothetical planet around a star, with a given set of parameters (a, i, e, Ω, ω, τ, M, and Π). We calculate the position x in each image i using Kepler’s laws, and measure the flux at that location as L _x,i . We then calculate σ _x,i , the uncertainty in L _x,i , by measuring the contrast in an annulus at that separation from the matching backward-rotated image. L _x,i is then compared to the model parameter L, which is the same for all epochs using the likelihood function given by equation N.