Revealing the relation between black-hole growth and host-galaxy compactness among star-forming galaxies. (arXiv:2007.04987v1 [astro-ph.GA])

Revealing the relation between black-hole growth and host-galaxy compactness among star-forming galaxies. (arXiv:2007.04987v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ni_Q/0/1/0/all/0/1">Q. Ni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandt_W/0/1/0/all/0/1">W. N. Brandt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_G/0/1/0/all/0/1">G. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leja_J/0/1/0/all/0/1">J. Leja</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C.-T. J. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_B/0/1/0/all/0/1">B. Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matharu_J/0/1/0/all/0/1">J. Matharu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_M/0/1/0/all/0/1">M. Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vito_F/0/1/0/all/0/1">F. Vito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xue_Y/0/1/0/all/0/1">Y. Q. Xue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_K/0/1/0/all/0/1">K. Zhang</a>

Recent studies show that a universal relation between black-hole (BH) growth
and stellar mass ($M_bigstar$) or star formation rate (SFR) is an
oversimplification of BH-galaxy co-evolution, 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 $approx 6300$ massive
galaxies with $I_{rm 814W}~<~24$ at $z$ $<$ 1.2 in the 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
$M_bigstar$ (or SFR). The projected central surface-mass density within 1 kpc,
$Sigma_{1}$, is utilized to represent host-galaxy compactness in our study. We
find that the $rm overline{BHAR}$-$Sigma_{1}$ relation is stronger than
either the $rm overline{BHAR}$-$M_bigstar$ or $rm overline{BHAR}$-SFR
relation among SF galaxies, and this $rm overline{BHAR}$-$Sigma_{1}$
relation applies to both bulge-dominated galaxies and galaxies that are not
dominated by bulges. This $rm overline{BHAR}$-$Sigma_{1}$ 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 $sim$ kpc of the galaxy. This
$rm overline{BHAR}$-$Sigma_{1}$ relation can also be interpreted as the
relation between BH growth and the central velocity dispersion of host galaxies
at a given gas content, indicating the role of the host-galaxy potential well
in feeding BHs.

Recent studies show that a universal relation between black-hole (BH) growth
and stellar mass ($M_bigstar$) or star formation rate (SFR) is an
oversimplification of BH-galaxy co-evolution, 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 $approx 6300$ massive
galaxies with $I_{rm 814W}~<~24$ at $z$ $<$ 1.2 in the 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
$M_bigstar$ (or SFR). The projected central surface-mass density within 1 kpc,
$Sigma_{1}$, is utilized to represent host-galaxy compactness in our study. We
find that the $rm overline{BHAR}$-$Sigma_{1}$ relation is stronger than
either the $rm overline{BHAR}$-$M_bigstar$ or $rm overline{BHAR}$-SFR
relation among SF galaxies, and this $rm overline{BHAR}$-$Sigma_{1}$
relation applies to both bulge-dominated galaxies and galaxies that are not
dominated by bulges. This $rm overline{BHAR}$-$Sigma_{1}$ 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 $sim$ kpc of the galaxy. This
$rm overline{BHAR}$-$Sigma_{1}$ relation can also be interpreted as the
relation between BH growth and the central velocity dispersion of host galaxies
at a given gas content, indicating the role of the host-galaxy potential well
in feeding BHs.

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