Ni, Q.Q.NiBrandt, W. N.W. N.BrandtYang, G.G.YangLeja, J.J.LejaChen, C. -T. J.C. -T. J.ChenLuo, B.B.LuoMatharu, J.J.MatharuSun, M.M.SunVITO, FabioFabioVITOXue, Y. Q.Y. Q.XueZhang, K.K.Zhang2025-02-142025-02-1420210035-8711http://hdl.handle.net/20.500.12386/35953Recent studies show that a universal relation between black hole (BH) growth and stellar mass (M<SUB>⋆</SUB>) or star formation rate (SFR) is an oversimplification of BH-galaxy coevolution, and that morphological and structural properties of host galaxies must also be considered. Particularly, a possible connection between BH growth and host-galaxy compactness was identified among star-forming (SF) galaxies. Utilizing ≈6300 massive galaxies with I<SUB>814W</SUB> < 24 at z < 1.2 in the Cosmic Evolution Survey (COSMOS) field, we perform systematic partial correlation analyses to investigate how sample-averaged BH accretion rate ($\rm \overline{BHAR}$) depends on host-galaxy compactness among SF galaxies, when controlling for morphology and M<SUB>⋆</SUB> (or SFR). The projected central surface mass density within 1 kpc, Σ<SUB>1</SUB>, is utilized to represent host-galaxy compactness in our study. We find that the $\rm \overline{BHAR}$-Σ<SUB>1</SUB> relation is stronger than either the $\rm \overline{BHAR}$-M<SUB>⋆</SUB> or $\rm \overline{BHAR}$-SFR relation among SF galaxies, and this $\rm \overline{BHAR}$-Σ<SUB>1</SUB> relation applies to both bulge-dominated galaxies and galaxies that are not dominated by bulges. This $\rm \overline{BHAR}$-Σ<SUB>1</SUB> relation among SF galaxies suggests a link between BH growth and the central gas density of host galaxies on the kpc scale, which may further imply a common origin of the gas in the vicinity of the BH and in the central ~kpc of the galaxy. This $\rm \overline{BHAR}$-Σ<SUB>1</SUB> relation can also be interpreted as the relation between BH growth and the central velocity dispersion of host galaxies at a given gas content (i.e. gas mass fraction), indicating the role of the host-galaxy potential well in regulating accretion on to the BH.STAMPAenArticle10.1093/mnras/staa35142-s2.0-85099681417https://academic.oup.com/mnras/article/500/4/4989/59816352021MNRAS.500.4989NFIS/05 - ASTRONOMIA E ASTROFISICA