Browsing by Author "Sun, M."

Now showing 1 - 2 of 2
  • Thumbnail Image
    Item
    Black Hole Growth Is Mainly Linked to Host-galaxy Stellar Mass Rather Than Star Formation Rate
    (2017) Wang, J.; Yang, G.; Chen, C.; Vito, F.; Brandt, W.; Alexander, D.; Luo, B.; Sun, M.; Xue, Y.; Bauer, Franz Erik; Koekemoer, A.; Lehmer, B.; Liu, T.; Schneider, D.; Shemmer, O.; Trump J.; Vignali, C.
  • No Thumbnail Available
    Item
    Revealing the relation between black hole growth and host-galaxy compactness among star-forming galaxies
    (2021) Ni, Q.; Brandt, W. N.; Yang, G.; Leja, J.; Chen, C-T J.; Luo, B.; Matharu, J.; Sun, M.; Vito, F.; Xue, Y. Q.; Zhang, K.
    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 approximate to 6300 massive galaxies with I-814W < 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, Sigma(1), is utilized to represent host-galaxy compactness in our study. We find that the BHAR-Sigma(1) relation is stronger than either the BHAR-M-* or BHAR-SFR relation among SF galaxies, and this BHAR-Sigma(1) relation applies to both bulge-dominated galaxies and galaxies that are not dominated by bulges. This 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 similar to kpc of the galaxy. This 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 (i.e. gas mass fraction), indicating the role of the host-galaxy potential well in regulating accretion on to the BH.