The angular momentum-mass relation: A fundamental law from dwarf irregulars to massive spirals

In a Λ CDM Universe, the specific stellar angular momentum (j_∗) and stellar mass (M_∗) of a galaxy are correlated as a consequence of the scaling existing for dark matter haloes (j_h ∞ ^{2/ 3}). The shape of this law is crucial to test galaxy formation models, which are currently discrepant especially at the lowest masses, allowing to constrain fundamental parameters, such as, for example, the retained fraction of angular momentum. In this study, we accurately determine the empirical j_∗-M_∗ relation (Fall relation) for 92 nearby spiral galaxies (from S0 to Irr) selected from the Spitzer Photometry and Accurate Rotation Curves (SPARC) sample in the unprecedented mass range 7 ≤ log M_∗/ M_⊙≤ 11.5. We significantly improve all previous estimates of the Fall relation by determining j_∗ profiles homogeneously for all galaxies, using extended HI rotation curves, and selecting only galaxies for which a robust j_∗ could be measured (converged j_∗(<R) radial profile). We find the relation to be well described by a single, unbroken power-law j_∗ α M_∗^α over the entire mass range, with α = 0.55 ± 0.02 and orthogonal intrinsic scatter of 0.17 ± 0.01 dex. We finally discuss some implications of this fundamental scaling law for galaxy formation models and, in particular, the fact that it excludes models in which discs of all masses retain the same fraction of the halo angular momentum.