We present radial density profiles, as traced by luminous galaxies and dark
matter particles, for voids in eleven snapshots of the \texttt{TNG300}
simulation. The snapshots span 11.65~Gyr of cosmic time, corresponding to the
redshift range $0 \le z \le 3$. Using the comoving galaxy fields, voids were
identified via a well-tested, watershed transformation-based algorithm. Voids
were defined to be underdense regions that are unlikely to have arisen from
Poisson noise, resulting in the selection of $\sim100-200$ of the largest
underdense regions in each snapshot. At all redshifts, the radial density
profiles as traced by both the galaxies and the dark matter resemble inverse
top-hat functions. Tuttavia, details of the functions (particularly the
underdensities of the innermost regions and the overdensities of the ridges)
evolve considerably more for the dark matter density profiles than for the
galaxy density profiles. At all redshifts, a linear relationship between the
galaxy and dark matter density profiles exists, and the slope of the
relationship is similar to the bias estimates for \texttt{TNG300} snapshots.
Lastly, we identify distinct environments in which voids can exist, defining
“void-in-void” E “void-in-cloud” populations (i.e., voids that reside in
larger underdense or overdense regions, respectively) and we investigate ways
in which the relative densities of dark matter and galaxies in the interiors
and ridges of these structures vary as a function of void environment.

Questo articolo esplora i giri e le loro implicazioni.

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