Fig. 1: Comparison between the relations of μHI to M⋆ and μHI to MBH for the BH sample.
From: Black holes regulate cool gas accretion in massive galaxies
a,b, μHI–M⋆ (a) and μHI–MBH (b) correlations. Galaxies are colour-coded by their morphological T types, with smaller values being more early-type and larger values more late-type morphologies. The orange lines represent the best-fitted linear relation, taking into account the uncertainties of both variables. c,d, Comparison of the partial correlation of μHI–M⋆ (while controlling for MBH) (c) and μHI–MBH (while controlling for M⋆) (d). The x- and y-axes show the residual in μHI and M⋆ after removing their dependence on MBH in the left panel, and MBH after removing their dependence on M⋆ in the right panel: Δlog μHI = log μHI − log μHI(MBH) and Δlog M⋆ = log M⋆ − log M⋆(MBH) in the left panel, and Δlog μHI = log μHI − log μHI(M⋆) and Δlog MBH = log MBH − log MBH(M⋆) in the right panel. The horizontal dashed line indicates zero correlation, that is, there is no intrinsic correlation between the two quantities. The Spearman correlation coefficients between the two corresponding variables are shown in each panel. The error bars refer to 1σ measurement errors.
