TY - JOUR
T1 - Revealing the relation between black hole growth and host-galaxy compactness among star-forming galaxies
AU - Ni, Q.
AU - Brandt, W. N.
AU - Yang, G.
AU - Leja, J.
AU - Chen, C. T.J.
AU - Luo, B.
AU - Matharu, J.
AU - Sun, M.
AU - Vito, F.
AU - Xue, Y. Q.
AU - Zhang, K.
N1 - Publisher Copyright:
© 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2021/2/1
Y1 - 2021/2/1
N2 - Recent studies show that a universal relation between black hole (BH) growth and stellar mass (M∗) 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 I814W < 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 (BHAR) depends on host-galaxy compactness among SF galaxies, when controlling for morphology and M∗ (or SFR). The projected central surface mass density within 1 kpc, ς1, is utilized to represent host-galaxy compactness in our study. We find that the BHAR-ς1 relation is stronger than either the BHAR-M∗ or BHAR-SFR relation among SF galaxies, and this BHAR-ς1 relation applies to both bulge-dominated galaxies and galaxies that are not dominated by bulges. This BHAR-ς1 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 BHAR-ς1 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.
AB - Recent studies show that a universal relation between black hole (BH) growth and stellar mass (M∗) 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 I814W < 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 (BHAR) depends on host-galaxy compactness among SF galaxies, when controlling for morphology and M∗ (or SFR). The projected central surface mass density within 1 kpc, ς1, is utilized to represent host-galaxy compactness in our study. We find that the BHAR-ς1 relation is stronger than either the BHAR-M∗ or BHAR-SFR relation among SF galaxies, and this BHAR-ς1 relation applies to both bulge-dominated galaxies and galaxies that are not dominated by bulges. This BHAR-ς1 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 BHAR-ς1 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.
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U2 - 10.1093/mnras/staa3514
DO - 10.1093/mnras/staa3514
M3 - Article
AN - SCOPUS:85099681417
SN - 0035-8711
VL - 500
SP - 4989
EP - 5008
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -