  Traditionally the spherical collapse of objects is studied with respect to a
uniform background density, yielding the critical over-density
$\delta_\mathrm{c}$ as key ingredient to the mass function of virialized
objects. Here we investigate the shear and rotation acting on a peak in a
Gaussian random field. By assuming that collapsing objects mainly form at those
peaks, we use this shear and rotation as external effects changing the dynamics
of the spherical collapse, which is described by the Raychaudhuri equation. We
therefore assume that the shear and rotation have no additional dynamics on top
of their cosmological evolution and thus only appear as inhomogeneities in the
differential equation.
