The Origin of the Relation Between Stellar Angular Momentum and Stellar Mass in Nearby Disk-dominated galaxies

Abstract

The IllustrisTNG simulations reproduce the observed scaling relation between stellar specific angular momentum (sAM) $j_{\mathrm{s}}$ and mass $M_{\mathrm{s}}$ of central galaxies. We show that the local $j_{\mathrm{s}}$-$M_{\mathrm{s}}$ relation $\log j_{\mathrm{s}}=0.55\log M_{\mathrm{s}}+2.77$ develops at $z\lesssim 1$ in disk-dominated galaxies. We provide a simple model that describes well such a connection between halos and galaxies. The index 0.55 of the $j_{\mathrm{s}}$-$M_{\mathrm{s}}$ relation comes from the product of the indices of the $j_{\mathrm{tot}}\propto M_{\mathrm{tot}}^{0.81}$, $M_{\mathrm{tot}}\propto M_{\mathrm{s}}^{0.67}$, and $j_{\mathrm{s}}\propto j_{\mathrm{tot}}$ relations, where $j_{\mathrm{tot}}$ and $M_{\mathrm{tot}}$ are overall sAM and mass of a halo. A non-negligible deviation from the tidal torque theory, which predicts $j_{\mathrm{tot}}\propto M_{\mathrm{tot}}^{2/3}$, should be included. This model further suggests that the stellar-to-halo mass ratio of disk galaxies increases monotonically following a nearly power-law function that is consistent with the latest dynamical measurements. Biased collapse, in which galaxies form from the inner and lower sAM portion of their parent halos, has a minor effect at low redshifts. The retention factor of angular momentum reaches $\sim 1$ in disk galaxies with strong rotations, and it correlates inversely with the mass fraction of the spheroidal component, which partially explains the morphological dependence of the $j_{\mathrm{s}}$-$M_{\mathrm{s}}$ relation.

10 pages, 5 figures, accpeted for publication on ApJL

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• The Physical Origin of the Mass-Size Relation and Its Scatter of Disk Galaxies
• IllustrisTNG Insights: Factors Affecting the Presence of Bars in Disk Galaxies
• Mass-morphology relation of TNG50 galaxies
• Spin speed correlations and the evolution of galaxy-halo systems
• Negligible Effects of Baryons on the Angular Momentum Scaling Relations of Galactic Dark Matter Halos
• A Shallow Slope for the Stellar Mass--Angular Momentum Relation of Star-Forming Galaxies at $1.5<z<2.5$
• Exploring the Angular Momentum -- Atomic Gas Content Connection with EAGLE and IllustrisTNG