# A survey of the thermal and non-thermal properties of cosmic filaments

## TL;DR

This survey analyzes cosmological simulations to understand the thermal and magnetic properties of cosmic filaments, revealing how different physical processes influence the intergalactic medium's characteristics.

## Contribution

It provides a comprehensive analysis of filament properties under various baryonic physics and magnetogenesis scenarios using high-resolution simulations.

## Key findings

- Non-gravitational physics has modest impact on filament thermodynamics.
- Magnetic properties vary significantly with seeding scenarios.
- Correlations exist between halo properties and filament environment.

## Abstract

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.