Characterising HOD in filaments and nodes of the cosmic web. (arXiv:2310.19928v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Perez_N/0/1/0/all/0/1">Noelia R. Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pereyra_L/0/1/0/all/0/1">Luis A. Pereyra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coldwell_G/0/1/0/all/0/1">Georgina Coldwell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_F/0/1/0/all/0/1">Facundo Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alfaro_I/0/1/0/all/0/1">Ignacio G. Alfaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruiz_A/0/1/0/all/0/1">Andrés N. Ruiz</a>
The standard paradigm for the formation of the Universe suggests that large
structures are formed from hierarchical clustering by the continuous accretion
of less massive galaxy systems through filaments. In this context, filamentary
structures play an important role in the properties and evolution of galaxies
by connecting high-density regions, such as nodes, and being surrounded by
low-density regions, such as cosmic voids. The availability of the filament and
point critic catalogues extracted by textsc{DisPerSE} from the
textsc{Illustris} TNG300-1 hydrodynamic simulation allows a detailed analysis
of these structures. The halo occupation distribution (HOD) is a powerful tool
for linking galaxies and dark matter halos, allowing constrained models of
galaxy formation and evolution. In this work we combine the advantage of halo
occupancy with information from the filament network to analyse the HOD in
filaments and nodes. In our study, we distinguish the inner regions of cosmic
filaments and nodes from their surroundings. The results show that the
filamentary structures have a similar trend to the total galaxy sample
indicating that, although the filaments span a wide range of densities, they
may represent regions of average density. In the case of the nodes sample, an
excess of faint and blue galaxies is found for the low-mass nodes suggesting
that these structures are not virialised and that galaxies may be continuously
falling through the filaments. Instead, the higher-mass halos could be in a
more advanced stage of evolution showing features of virialised structures.
The standard paradigm for the formation of the Universe suggests that large
structures are formed from hierarchical clustering by the continuous accretion
of less massive galaxy systems through filaments. In this context, filamentary
structures play an important role in the properties and evolution of galaxies
by connecting high-density regions, such as nodes, and being surrounded by
low-density regions, such as cosmic voids. The availability of the filament and
point critic catalogues extracted by textsc{DisPerSE} from the
textsc{Illustris} TNG300-1 hydrodynamic simulation allows a detailed analysis
of these structures. The halo occupation distribution (HOD) is a powerful tool
for linking galaxies and dark matter halos, allowing constrained models of
galaxy formation and evolution. In this work we combine the advantage of halo
occupancy with information from the filament network to analyse the HOD in
filaments and nodes. In our study, we distinguish the inner regions of cosmic
filaments and nodes from their surroundings. The results show that the
filamentary structures have a similar trend to the total galaxy sample
indicating that, although the filaments span a wide range of densities, they
may represent regions of average density. In the case of the nodes sample, an
excess of faint and blue galaxies is found for the low-mass nodes suggesting
that these structures are not virialised and that galaxies may be continuously
falling through the filaments. Instead, the higher-mass halos could be in a
more advanced stage of evolution showing features of virialised structures.
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