Fig. 3: The impact of MBH on the correlation between μHI and other main galactic parameters.
From: Black holes regulate cool gas accretion in massive galaxies
a–e, The HI-detection fraction along MBH (a) and some other main physical parameters of galaxies, including M⋆ (b), Σstar (c), Mbulge (d) and SSFR (e). The vertical dashed lines indicate the position at which the HI-detection rates hit 60%. f–j, The relation between the parameters MBH (f), M⋆ (g), Σstar (h), Mbulge (i) and SSFR (j) and μHI. The contours denote the distribution of the HI-detected galaxy sample, whereas the filled red circles denote the BH sample with 1σ error bars. The best-fitted μHI–MBH relations for the HI-detected galaxy sample and the BH sample are shown in f by the black and orange lines, respectively. The median 1σ error bars for the galaxy sample are shown. k–n, The relation between the residual in μHI and the residual in other galactic parameters after removing their dependence on MBH: Δlog μHI = log μHI − log μHI(MBH) and Δlog X = log X − log X(MBH) with X representing M⋆ (k), Σstar (l), Mbulge (m) and SSFR (n), and μHI(MBH) and X(MBH) derived from their best-fitted relation with MBH (Extended Data Fig. 2). The solid medium-blue lines in k–n show the running median of the residuals in μHI. The Spearman correlation coefficients for the HI-detected galaxy sample between the corresponding x and y variables are shown in f–n.
