The baryonic specific angular momentum of disc galaxies
arXiv:2009.06645 · doi:10.1051/0004-6361/202039340
Abstract
(Abridged) Specific angular momentum is one of the key parameters that control the evolution of galaxies. We derive the baryonic specific angular momentum of disc galaxies and study its relation with the dark matter specific angular momentum. Using a combination of high-quality HI rotation curves and HI/near-IR surface densities, we homogeneously measure the stellar () and gas () specific angular momenta for a large sample of local disc galaxies. This allows us to determine the baryonic specific angular momentum () with high accuracy and across a very wide range of masses. The relation is an unbroken power-law from log(/, with slope . For the gas component, we find that the relation is also an unbroken power-law from log(/, with a steeper slope of . Regarding the baryonic relation, our data support a correlation characterized by single power-law with slope . Our most massive spirals and smallest dwarfs lie along the same sequence. While the relations are tight and unbroken, we find internal correlations inside them: At fixed , galaxies with larger have larger disc scale lengths, and at fixed , gas-poor galaxies have lower than expected. We estimate the retained fraction of baryonic specific angular momentum, finding it constant across our entire mass range with a value of , indicating that the of present-day disc galaxies is comparable to the initial specific angular momentum of their dark matter haloes. These results set important constraints for hydrodynamical simulations and semi-analytical models aiming to reproduce galaxies with realistic specific angular momenta.
Matching the published version of January (2021A&A...647A..76M) The full version of the main table is available at https://www.dropbox.com/s/xizhjqiuahqbdtp/tbsam.dat
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