Baryonic Imprints on DM Halos: Population Statistics from Dwarf Galaxies
  to Galaxy Clusters
  In a purely cold dark matter universe, the initial matter power spectrum and
its subsequent gravitational growth contain no special mass- or time-scales,
and so neither do the emergent population statistics of internal dark matter
(DM) halo properties. Using 1.5 million halos from three IllustrisTNG
realizations of a LambdaCDM universe, we show that galaxy formation physics
drives non-monotonic features ("wiggles") into DM property statistics across
six decades in halo mass, from dwarf galaxies to galaxy clusters. We
characterize these features by extracting the halo mass-dependent statistics of
five DM halo properties -- velocity dispersion, NFW concentration, density- and
velocity-space shapes, and formation time -- using kernel-localized linear
regression (KLLR). Comparing precise estimates of normalizations, slopes, and
covariances between realizations with and without galaxy formation, we find
systematic deviations across all mass-scales, with maximum deviations of 25% at
the Milky-Way mass of 1e12 Msun. The mass-dependence of the wiggles is set by
the interplay between different cooling and feedback mechanisms, and we discuss
its observational implications. The property covariances depend strongly on
halo mass and physics treatment, but the correlations are mostly robust. Using
multivariate KLLR and interpretable machine learning, we show the halo
concentration and velocity-space shape are principal contributors, at different
mass, to the velocity dispersion variance. Statistics of mass accretion rate
and DM surface pressure energy are provided in an appendix. We publicly release
halo property catalogs and KLLR parameters for the TNG runs at twenty epochs up
to z = 12.
