Black-Hole Growth is Mainly Linked to Host-Galaxy Stellar Mass rather than Star Formation Rate

Abstract

We investigate the dependence of black-hole accretion rate (BHAR) on host-galaxy star formation rate (SFR) and stellar mass ($M_{\ast }$) in the CANDELS/GOODS-South field in the redshift range of $0.5\le z<2.0$. Our sample consists of $\approx 18000$ galaxies, allowing us to probe galaxies with $0.1\lesssim \mathrm{SFR}\lesssim 100M_{\odot }{\mathrm{yr}}^{-1}$ and/or $10^8\lesssim M_{\ast }\lesssim 10^{11}{M}_{\odot }$. We use sample-mean BHAR to approximate long-term average BHAR. Our sample-mean BHARs are derived from the $Chandra$ Deep Field-South 7 Ms observations, while the SFRs and $M_{\ast }$ have been estimated by the CANDELS team through SED fitting. The average BHAR is correlated positively with both SFR and $M_{\ast }$, and the BHAR-SFR and BHAR-$M_{\ast }$ relations can both be described acceptably by linear models with a slope of unity. However, BHAR appears to be correlated more strongly with $M_{\ast }$ than SFR. This result indicates that $M_{\ast }$ is the primary host-galaxy property related to black-hole growth, and the apparent BHAR-SFR relation is largely a secondary effect due to the star-forming main sequence. Among our sources, massive galaxies ($M_{\ast }\gtrsim 10^{10}{M}_{\odot }$) have significantly higher BHAR/SFR ratios than less-massive galaxies, indicating the former have higher black-hole fueling efficiency and/or higher SMBH occupation fraction than the latter. Our results can naturally explain the observed proportionality between $M_{\mathrm{BH}}$ and $M_{\ast }$ for local giant ellipticals, and suggest their $M_{\mathrm{BH}}/M_{\ast }$ is higher than that of local star-forming galaxies. Among local star-forming galaxies, massive systems might have higher $M_{\mathrm{BH}}/M_{\ast }$ compared to dwarfs.

18 pages, 11 figures, 3 tables; accepted for publication in ApJ

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