How to add massive neutrinos to your ΛCDM simulation - extending cosmology rescaling algorithms

Providing accurate predictions for the spatial distribution of matter and luminous tracers in the presence of massive neutrinos is an important task, given the imminent arrival of highly accurate large-scale structure observations. In this work, we address this challenge by extending cosmology-rescaling algorithms to massive neutrino cosmologies. In this way, a Lambda CDM simulation can be modified to provide non-linear structure formation predictions in the presence of a hot component of arbitrary mass, and, if desired, to include non-gravitational modifications to the clustering of matter on large scales. We test the accuracy of the method by comparing its predictions to a suite of simulations carried out explicitly including a neutrino component in its evolution equations. We find that, for neutrino masses in the range M.. [0.06, 0.3] eV thematter power spectrum is recovered to better than 1 per cent on all scales k< 2 h Mpc(-1). Similarly, the halo mass function is predicted at a few per cent level over the range Mhalo is an element of [10(12), 10(15)] h(-1) M-circle dot, and so do also the multipoles of the galaxy two-point correlation function in redshift space over r is an element of [0.1, 200] h(-1) Mpc. We provide parametric forms for the necessary transformations, as a function of Omega m and Omega nu for various target redshifts.