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The specific angular momenta ($j\equiv J/M$) of stars ($j_{\star}$), gas($j_{\mathrm{gas}}$), baryons as a whole ($j_{\mathrm{b}}$) and dark matterhaloes ($j_{\mathrm{h}}$) contain clues of vital importance about how galaxiesform and evolve. Using one of the largest samples of disc galaxies (S0-BCD)with high-quality rotation curves and near-infrared surface photometry, weperform a detailed comparative analysis of $j$ that stretches across a varietyof galaxy properties. Our analysis imposes tight constraints on the "retained"fractions of specific angular momentum ($j_{\star}/j_{\mathrm{h}}$,$j_{\mathrm{HI}}/j_{\mathrm{h}}$ and $j_{\mathrm{b}}/j_{\mathrm{h}}$), as wellas on their systematic trends with mass fraction and galaxy morphology, thus onhow well specific angular momentum is conserved in the process of disc galaxyformation and evolution. In particular, one of the most innovative results ofour analysis is the finding that galaxies with larger baryon fractions havealso retained larger fractions of their specific angular momentum. Furthermore,our analysis demonstrates how challenging it is to characterize barred galaxiesfrom a gravitational instability point of view. This is true not only for thepopular Efstathiou, Lake & Negroponte bar instability criterion, which fails toseparate barred from non-barred galaxies in about 55% of the cases, but alsofor the mass-weighted Toomre parameter of atomic gas, $\langleQ_{\mathrm{HI}}\rangle$, which succeeds in separating barred from non-barredgalaxies, but only in a statistical sense.

The specific angular momentum of disc galaxies and its connection with galaxy morphology, bar structure and disc gravitational instability