Baryonic Imprints on DM Halos: the concentration-mass relation and its dependence on 28 model parameters in the CAMELS suite

The evolution of baryons in halos, as well as their gravitational impact on the total-matter phase space, has a rich phenomenology and is vital in answering many questions in both cosmology and astrophysics. We use the CAMELS simulation suite to quantify the impact of twenty-three different galaxy formation parameters/processes (as well as five cosmological parameters) on the concentration–mass relation, $c_{\mathrm{v}\mathrm{i}\mathrm{r}}$ - $M_{\mathrm{v}\mathrm{i}\mathrm{r}}$, which characterizes the radial density distribution in halos. We construct a simulation-informed nonlinear model for concentration as a function of halo mass, redshift, and twenty-eight cosmological/astrophysical parameters. This is done using 2048 simulations of the IllustrisTNG galaxy formation model from the CAMELS suite. We extract the imprints of galaxy formation across a wide range in mass $M_{\mathrm{v}\mathrm{i}\mathrm{r}}\in [{10}^{11},{10}^{14.5}]$ $M_{\odot }\mathrm{/}h$ and in redshift $z\in [0,3]$, finding clear mass- and redshift-dependent features in each of the different feedback mechanisms. From our measurements, we construct a three-component phenomenological model that can include astrophysical imprints in the concentration–mass relation in a fast and simple manner.