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Providing accurate predictions for the spatial distribution of matter andluminous tracers in the presence of massive neutrinos is an important task,given the imminent arrival of highly accurate large-scale structureobservations. In this work, we address this challenge by extendingcosmology-rescaling algorithms to massive neutrino cosmologies. In this way, a$\Lambda$CDM simulation can be modified to provide nonlinear structureformation predictions in the presence a hot component of arbitrary mass, and,if desired, to include non-gravitational modifications to the clustering ofmatter on large scales. We test the accuracy of the method by comparing itspredictions to a suite of simulations carried out explicitly including aneutrino component in its evolution equations. We find that, for neutrinomasses in the range $M_\nu \in [0.06, 0.3] ~ \mathrm{eV}$ the matter powerspectrum is recovered to better than $1\%$ on all scales$k<2~h~\mathrm{Mpc}^{-1}$. Similarly, the halo mass function is predicted at afew percent level over the range $M_{\rm halo} \in [10^{12}, 10^{15}] ~ h^{-1}~ \mathrm{M}_{\odot}$, and so do also the multipoles of the galaxy 2-pointcorrelation function in redshift space over $r \in [0.1, 200] ~ h^{-1} ~\mathrm{Mpc}$. We provide parametric forms for the necessary transformations,as a function of $\Omega_{\rm m}$ and $\Omega_{\nu}$ for various targetredshifts.

How to add massive neutrinos to your $\Lambda$CDM simulation -- extending cosmology rescaling algorithms