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We explore fundamental properties of the distribution of low mass dark matterhalos within the cosmic web using warm dark matter (WDM) and cold dark matter(CDM) cosmological simulations. Using self abundance-matched mock galaxycatalogs, we show that the distribution of dwarf galaxies in a WDM universe,wherein low mass halo formation is heavily suppressed, is nearlyindistinguishable to that of a CDM universe whose low mass halos are not seenbecause galaxy formation is suppressed below some threshold halo mass. However,if the scatter between dwarf galaxy luminosity and halo properties is largeenough, low mass CDM halos would sometimes host relatively bright galaxiesthereby populating CDM voids with the occasional isolated galaxy and reducingthe numbers of completely empty voids. Otherwise, without high mass to lightscatter, all mock galaxy clustering statistics that we consider--theauto-correlation function, the numbers and radial profiles of satellites, thenumbers of isolated galaxies, and the PDF of small voids--are nearly identicalin CDM and WDM. WDM voids are neither larger nor emptier than CDM voids, whenconstructed from abundance-matched halo catalogs. It is thus a challenge todetermine whether the CDM problem of the over-abundance of small halos withrespect to the number density of observed dwarf galaxies has a cosmologicalsolution or an astrophysical solution. However, some clues about the darkmatter particle and the scatter between the properties of dwarf galaxies andtheir dark matter halo hosts might be found in the cosmic web of galaxies infuture surveys of the local volume.

The same with less: The cosmic web of warm versus cold dark matter dwarf galaxies