Much ado about nothing: Galaxy formation and galactic outflows in cosmic voids

We present a theoretical framework for calculating the volume filling fraction of galactic outflows in cosmic voids by integrating analytical models for the halo mass function (HMF), the halo occupation fraction, the SMHM relation, and outflow sizes. Using ramses, we perform a hydrodynamical zoom-in simulation of the central 25 cMpc h-1 region of a spherical void, identified as the lowest density region among 1000 random spheres in a parent 1 Gpc box simulation. This void has a diameter of 120 cMpc h-1 and a density contrast of. We find that the properties of void galaxies remain stable when expanding the zoom-in region to 50 cMpc h-1, though our relatively low-mass resolution impacts the results. Our higher resolution simulation aligns with the analytical HMF that accounts for the void's underdensity and size. While higher resolution improves stellar mass estimates for low-mass haloes, computational constraints necessitate a theoretical framework that enables extrapolation to infinite resolution. Our analytical model, calibrated to our simulations, enables extrapolation down to the filtering mass of star-forming haloes. To compare galaxy properties in this void with those in the field, we conduct a companion field simulation of the same box size. At infinite resolution, we predict wind volume filling fractions of 18.6 per cent in the field and 3.1 per cent in our void, with values dependent on cosmic variance, void size, and underdensity. Dwarf galaxies contribute minimally, and resolving haloes to suffices for robust estimates. Applying our framework to the Local Group void (,), we predict a wind volume filling fraction of.