  We measure the large-scale bias of dark matter halos in simulations with
non-Gaussian initial conditions of the local type, and compare this bias to the
response of the mass function to a change in the primordial amplitude of
fluctuations. The two are found to be consistent, as expected from physical
arguments, for three halo-finder algorithms which use different Spherical
Overdensity (SO) and Friends-of-Friends (FoF) methods. On the other hand, we
find that the commonly used prediction for universal mass functions, that the
scale-dependent bias is proportional to the first-order Gaussian Lagrangian
bias, does not yield a good agreement with the measurements. For all halo
finders, high-mass halos show a non-Gaussian bias suppressed by 10-15% relative
to the universal mass function prediction. For SO halos, this deviation changes
sign at low masses, where the non-Gaussian bias becomes larger than the
universal prediction.
