  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 nonlinear structure
formation predictions in the presence 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 $M_\nu \in [0.06, 0.3] ~ \mathrm{eV}$ the matter power
spectrum is recovered to better than $1\%$ on all scales
$k<2~h~\mathrm{Mpc}^{-1}$. Similarly, the halo mass function is predicted at a
few 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-point
correlation 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 target
redshifts.
