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tokens: statistical studies that can identify correlations over longer time-scales, and more accurately measure the scatter between gas reservoirs and black hole growth. It is thus interesting to make predictions for the connection between H i and black hole properties. Fig. 9 shows how black hole properties depend on the H i content of galaxies in simba , specifically the total H i mass M H i (left column), and the H i mass fraction f H i = M H i / M * (right column). The rows show various black hole properties, from top to bottom: M BH , , M BH / M ⋆ , and f Edd . All galaxies are colour coded by sSFR. The running median at z = 0 is shown as the black line with 1σ uncertainties from jackknife resampling. The blue and turqoise lines show the running medians at z = 1, 2 respectively; the individual galaxy points are not shown at those redshifts. Figure 9. Black hole properties as a function of H i content in simba . Each galaxy at z = 0 is colour coded by sSFR and the black line is the running median at z = 0. The blue and cyan lines show the corresponding medians at z = 1, 2, respectively. There is a strong anticorrelation between M BH and f H i , as well as a correlation between f Edd and f H i , both reflecting a tight M BH – M ⋆ relation. The top left panel shows that the black hole mass is essentially uncorrelated with H i mass, and there is little evolution in this relation. More interestingly, at a given H i mass, larger black holes populate more quiescent galaxies. This shows that there is a strong connection between black hole growth and gas removal in galaxy outskirts, likely owing to suppression of cooling to feed the H i reservoir. The most star-forming galaxies primarily have the lowest M BH , but there is also a weaker trend that they have the highest M H i . Hence star formation is enhanced in galaxies that have both small black holes and high gas content. The top right panel shows M BH versus f H i , which displays a strong anticorrelation, reflecting a tight M BH – M ⋆ relation at late times, with the most star-forming galaxies having concurrently the smallest black holes and highest gas fractions. There is modest evolution upwards in this relation with time, such that galaxies at a given black hole mass have higher f H i at earlier times, reflecting the overall increase in gas content in galaxies at earlier epochs (Davé et al. 2019 ). The second row shows the dependence of BHAR on H i content. At z = 0, BHAR shows little correlation with H i mass, but there is an evident correlation at such that black hole accretion is stronger for higher H i masses. At these earlier epochs, the accretion is dominated by the torque-limited mode, which depends on gas fraction. Even though torque-limited accretion is computed within the core of the galaxy while the H i is more diffusely distributed, the overall enhanced gas content appears to drive black hole accretion. By z = 0, in contrast, the emergence of quenched galaxies dominated by Bondi