A survey of the thermal and non-thermal properties of cosmic filaments
  In this paper, we exploit a large suite of {\enzo} cosmological
magneto-hydrodynamical simulations adopting uniform mesh resolution, to
investigate the properties of cosmic filaments under different baryonic physics
and magnetogenesis scenarios. We exploit a isovolume based algorithm to
identify filaments and determine their attributes from the continuous
distribution of gas mass density in the simulated volumes. The global (e.g.
mass, size, mean temperature and magnetic field strength, enclosed baryon
fraction) and internal (e.g. density, temperature, velocity and magnetic field
profiles) properties of filaments in our volume are calculated across almost
four orders of magnitude in mass. The inclusion of variations in
non-gravitational physical processes (radiative cooling, star formation,
feedback from star forming regions and active galactic nuclei) as well as in
the seeding scenarios for magnetic fields (early magnetisation by primordial
process vs later seeding by galaxies) allows us to study both the large-scale
thermodynamics and the magnetic properties of the Warm-Hot Intergalactic Medium
(WHIM) with an unprecedented detail. We show how the impact of
non-gravitational physics on the global thermodynamical properties of filaments
is modest, with the exception of the densest gas environment surrounding
galaxies in filaments. Conversely, the magnetic properties of the WHIM in
filament are found to dramatically vary as different seeding scenarios are
considered. We study the correlation between the properties of galaxy-sized
halos and their host filaments, as well as between the halos and the local WHIM
in which they lie. Significant general statistical trends are reported.
