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In $\Lambda$CDM cosmology, to first order, galaxies form out of the coolingof baryons within the virial radius of their dark matter halo. The fractions ofmass and angular momentum retained in the baryonic and stellar components ofdisc galaxies put strong constraints on our understanding of galaxy formation.In this work, we derive the fraction of angular momentum retained in thestellar component of spirals, $f_j$, the global star formation efficiency$f_M$, and the ratio of the asymptotic circular velocity ($V_{\rm flat}$) tothe virial velocity $f_V$, and their scatter, by fitting simultaneously theobserved stellar mass-velocity (Tully-Fisher), size-mass, and mass-angularmomentum (Fall) relations. We compare the goodness of fit of three models: (i)where the logarithm of $f_j$, $f_M$, and $f_V$ vary linearly with the logarithmof the observable $V_{\rm flat}$; (ii) where these values vary as a doublepower law; and (iii) where these values also vary as a double power law butwith a prior imposed on $f_M$ such that it follows the expectations from widelyused abundance matching models. We conclude that the scatter in these fractionsis particularly small ($\sim 0.07$ dex) and that the linear model is by farstatistically preferred to that with abundance matching priors. This indicatesthat the fundamental galaxy formation parameters are small-scatter single-slopemonotonic functions of mass, instead of being complicated non-monotonicfunctions. This incidentally confirms that the most massive spiral galaxiesshould have turned nearly all the baryons associated with their haloes intostars. We call this the failed feedback problem.

Galaxy disc scaling relations: A tight linear galaxy -- halo connection challenges abundance matching