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We present a new set of galaxy scaling relations for the relative masscontent of atomic gas, molecular gas and stars. Such relations are driven bydisc gravitational instability, and originate from the low galaxy-to-galaxyvariance of Toomre's $Q$ stability parameter. We test such relations using morethan 100 galaxies, from massive spirals to dwarf irregulars, thus spanningseveral orders of magnitude in stellar mass($M_{\star}\approx10^{6\mbox{-}11}\,\mbox{M}_{\odot}$) and atomic gas mass($M_{\mathrm{HI}}\approx10^{7\mbox{-}10.5}\,\mbox{M}_{\odot}$). Such testsdemonstrate (i) that our scaling relations are physically motivated and tightlyconstrained, (ii) that the mass-averaged gravitational instability propertiesof galaxy discs are remarkably uniform across the sequence Sa-dIrr, and (iii)that specific angular momentum plays an important role in such a scenario.Besides providing new insights into a very important topic in galaxy evolution,this work provides a simple formula (Eq. 5) that one can use for generatingother galaxy relations driven by disc instability. We explain how to do that,mention a few possible applications, and stress the importance of testing ourapproach further.

From massive spirals to dwarf irregulars: a new set of tight scaling relations for cold gas and stars driven by disc gravitational instability