Osaka Feedback Model III: Cosmological Simulation CROCODILE. (arXiv:2401.06324v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Oku_Y/0/1/0/all/0/1">Yuri Oku</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagamine_K/0/1/0/all/0/1">Kentaro Nagamine</a>

We introduce our new cosmological simulation dataset CROCODILE, executed
using the GADGET4-Osaka smoothed particle hydrodynamics code. This simulation
incorporates an updated supernova (SN) feedback model of Oku et al. (2022) and
an active galactic nuclei (AGN) feedback model. A key innovation in our SN
feedback model is the integration of a metallicity- and redshift-dependent,
top-heavy IMF, which enables a higher energy injection rate per unit stellar
mass formed at high redshift. The CROCODILE dataset is comprehensive,
encompassing a variety of runs with diverse feedback parameters. This allows
for an in-depth exploration of the relative impacts of different feedback
processes in galactic evolution. Our initial comparisons with observational
data — spanning the galaxy stellar mass function, the star formation main
sequence, and the mass-metallicity relation — show promising agreement,
especially for the Fiducial run. These results establish a solid foundation for
our future work. We find that the SN feedback is a key driver in the chemical
enrichment of the IGM. Additionally, the AGN feedback creates metal-rich,
bipolar outflows that extend and enrich the CGM and IGM over a few Mpc scales.

We introduce our new cosmological simulation dataset CROCODILE, executed
using the GADGET4-Osaka smoothed particle hydrodynamics code. This simulation
incorporates an updated supernova (SN) feedback model of Oku et al. (2022) and
an active galactic nuclei (AGN) feedback model. A key innovation in our SN
feedback model is the integration of a metallicity- and redshift-dependent,
top-heavy IMF, which enables a higher energy injection rate per unit stellar
mass formed at high redshift. The CROCODILE dataset is comprehensive,
encompassing a variety of runs with diverse feedback parameters. This allows
for an in-depth exploration of the relative impacts of different feedback
processes in galactic evolution. Our initial comparisons with observational
data — spanning the galaxy stellar mass function, the star formation main
sequence, and the mass-metallicity relation — show promising agreement,
especially for the Fiducial run. These results establish a solid foundation for
our future work. We find that the SN feedback is a key driver in the chemical
enrichment of the IGM. Additionally, the AGN feedback creates metal-rich,
bipolar outflows that extend and enrich the CGM and IGM over a few Mpc scales.

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