Halo mass function and scale-dependent bias from N-body simulations with non-Gaussian initial conditions

摘要: We perform a series of high-resolution N-body simulations cosmological structure formation starting from Gaussian and non-Gaussian initial conditions. adopt the best-fitting parameters third- fifth-year data releases Wilkinson Microwave Anisotropy Probe, we consider non-Gaussianity local type parametrized by eight different values non-linearity parameter f NL . Building upon previous work based on case, show that, when expressed in terms suitable variables, mass function friends-of-friends haloes is approximately universal (i.e. independent redshift, cosmology matter transfer function) to good precision (nearly 10 per cent) also scenarios. provide fitting formulae for high-mass end (M > 13 h -1 M ⊙ ) , present non-universal fit bothfN L z be used applications requiring higher accuracy. For conditions, extend our wider range halo masses 2.4 x consistent linear bias. realistic power spectrum cosmologies departs 1 up 2 cent scales where baryonic-oscillation features are imprinted two-point statistics. Finally, using both halo-matter cross spectrum, confirm strong k-dependence bias large (k < 0.05 Mpc 1- which was already detected studies. However, find that commonly parametrizations peak-background split do not an accurate description extra dependencies wavenumber, and, possibly, clustering strength. simulation can as benchmark future determinations with galaxy surveys.