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We use a phenomenological model to show that black hole growth in the localUniverse (z < 0.1) can be described by two separate, mass independent Eddingtonratio distribution functions (ERDFs). We assume that black holes can be dividedinto two independent groups: those with radiatively efficient accretion,primarily hosted by optically blue and green galaxies, and those withradiatively inefficient accretion, which are mainly found in red galaxies. Withobserved galaxy stellar mass functions as input, we show that the observed AGNluminosity functions can be reproduced by using mass independent, broken powerlaw shaped ERDFs. We use the observed hard X-ray and 1.4 GHz radio luminosityfunctions to constrain the ERDF for radiatively efficient and inefficient AGN,respectively. We also test alternative ERDF shapes and mass dependent models.Our results are consistent with a mass independent AGN fraction and AGN hostsbeing randomly drawn from the galaxy population. We argue that the ERDF is notshaped by galaxy-scale effects, but by how efficiently material can betransported from the inner few parsecs to the accretion disc. Our results areincompatible with the simplest form of mass quenching where massive galaxieshost higher accretion rate AGN. Furthermore, if reaching a certain Eddingtonratio is a sufficient condition for maintenance mode, it can occur in all redgalaxies, not just the most massive ones.

AGN and their host galaxies in the local Universe: two mass independent Eddington ratio distribution functions characterize black hole growth