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Cosmic voids offer an extraordinary opportunity to study the effects ofmassive neutrinos on cosmological scales. Because they are freely streaming,neutrinos can penetrate the interior of voids more easily than cold dark matteror baryons, which makes their relative contribution to the mass budget in voidsmuch higher than elsewhere in the Universe. In simulations it has recently beenshown how various characteristics of voids in the matter distribution areaffected by neutrinos, such as their abundance, density profiles, dynamics, andclustering properties. However, the tracers used to identify voids inobservations (e.g., galaxies or halos) are affected by neutrinos as well, andisolating the unique neutrino signatures inherent to voids becomes moredifficult. In this paper we make use of the DEMNUni suite of simulations toinvestigate the clustering bias of voids in Fourier space as a function oftheir core density and compensation. We find a clear dependence on the sum ofneutrino masses that remains significant even for void statistics extractedfrom halos. In particular, we observe that the amplitude of the linear voidbias increases with neutrino mass for voids defined in dark matter, whereasthis trend gets reversed and slightly attenuated when measuring the relativevoid-halo bias using voids identified in the halo distribution. Finally, weargue how the original behaviour can be restored when considering observationsof the total matter distribution (e.g. via weak lensing), and comment onscale-dependent effects in the void bias that may provide additionalinformation on neutrinos in the future.

The bias of cosmic voids in the presence of massive neutrinos