In cosmological simulations without baryons, the relation between the specific angular momentum $j_{ \rm h}$ and mass $M_{ \rm h}$ of galactic dark matter halos has the well-established form $j_{ \rm h} \propto M_{ \rm h}^{ 2/3}$. This is invariably adopted as the starting point in efforts to understand the analogous relation between the specific angular momentum $j_{ \ast}$ and mass $M_{ \ast}$ of the stellar parts of galaxies, which are often re-expressed relative to the corresponding halo properties through the retention fractions $f_j = j_{ \ast} / j_{ \rm h}$ and $f_M = M_{ \ast} / M_{ \rm h}$. An important caveat here is that the adopted $j_{ \rm h} \propto M_{ \rm h}^{ 2/3}$ relation could, in principle, be modified by the gravitational back-reaction of baryons on dark matter (DM). We have tested for this possibility by comparing the $j_{ \rm h}$-$M_{ \rm h}$ relations in the IllustrisTNG100 and TNG50 simulations that include baryons (full-physics runs) with their counterparts that do not (DM-only runs). In all cases, we find scaling relations of the form $j_{ \rm h} \propto M_{ \rm h}^{ \alpha}$, with $\alpha \approx 2/3$ over the ranges of mass and redshift studied here: $M_{ \rm h} \geq 10^{ 10} \, M_{ \odot}$ and $0 \leq z \leq 2$. The values of $\alpha$ are virtually identical in the full-physics and DM-only runs at the same redshift. The only detectable effect of baryons on the $j_{ \rm h}$-$M_{ \rm h}$ relation is a slightly higher normalization, by 12%-15% at $z=0$ and by 5% at $z=2$. This implies that existing estimates of $f_j$ based on DM-only simulations should be adjusted downward by similar amounts. Finally, we discuss briefly some implications of this work for studies of galaxy formation.
Categories: astro-ph.GA astro-ph.CO
