Models of galaxy and halo clustering commonly assume that the tracers can be treated as a continuous field locally biased with respect to the underlying mass distribution. In the peak model pioneered by BBKS, one considers instead density maxima of the initial, Gaussian mass density field as an approximation to the formation site of virialized objects. However, because the peak constraint renders calculations almost prohibitive, all analytic studies of density peaks thus far have obtained results which are strictly valid at leading order and in Gaussian initial conditions solely. In this talk, I will show how the peak model can be extended to improve its predictive accuracy. I will apply the new results to study how the Lagrangian biasing and gravitational instability affect the scale-dependence of bias from small separations up to the Baryon Acoustic Oscillation scale.