Celiz, Bruno Martín
Argentina FaMAF – UNC
Galactic Stellar Haloes in ΛCDM simulations
Using the cosmological hydrodynamic simulation TNG50-1 we characterize stellar haloes (SHs) of galaxies with stellar mass in the range 8.0 < log M*/M☉ < 11.0 in a ΛCDM Universe. Defined as the stellar component at distances between twice the stellar half-mass radius (2r*) and the virial radius (r200), we studied the stellar mass (MSH), the size (rvir/2r*) and the spherically averaged density profile (ρ(r)) of isolated central galaxies’ SH at redshift z = 0 and analyzed their relation to intrinsic properties of the galaxy. We calculate the density profile’s logarithmic slope α, finding values -10 < α < -2 and that: i) strongly correlates with the SH mass fraction (fM); ii) is inversely proportional to the galaxy rotational support κrot; and iii) unlike what is reported in the literature, we do not find a tendency between the SHs slope α and the virial mass M200 for dwarfs galaxies. These results aim to predict and compare simulated and observed SHs properties for galaxies with mass lower than the Milky Way or Andromeda, suggesting that outer regions of galaxies could be good estimators of their intrinsic properties in a wide mass range.