Black Hole Growth Is Mainly Linked to Host-galaxy Stellar Mass Rather Than Star Formation Rate

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This article investigates the dependence of black hole accretion rate (BHAR) on host-galaxy star formation rate (SFR) and stellar mass in the CANDELS/GOODS-South field in the redshift range of 0.5 ⩽ z < 2.0.

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17 p.

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Yang, G.; Chen, C. -T. J.; Vito, F.; Brandt, William Nielsen; Alexander, David M.; Luo, Bin et al. June 15, 2017.

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This article investigates the dependence of black hole accretion rate (BHAR) on host-galaxy star formation rate (SFR) and stellar mass in the CANDELS/GOODS-South field in the redshift range of 0.5 ⩽ z < 2.0.

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17 p.

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Abstract: We investigate the dependence of black hole accretion rate (BHAR) on host-galaxy star formation rate (SFR) and stellar mass (M*) in the CANDELS/GOODS-South field in the redshift range of 0.5 ⩽ z < 2.0. Our sample consists of ≈18,000 galaxies, allowing us to probe galaxies with 0.1 M☉ yr-¹ ≲ SFR ≲ 100 M☉ yr-¹ and/or 10⁸ M☉ ≲ M∗ ≲ 10¹¹ M☉. 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∗ have been estimated by the CANDELS team through spectral energy distribution fitting. The average BHAR is correlated positively with both SFR and M∗, and the BHAR–SFR and BHAR–M* relations can both be described acceptably by linear models with a slope of unity. However, BHAR appears to be correlated more strongly with M* than SFR. This result indicates that M* is the primary host-galaxy property related to supermassive black hole (SMBH) 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∗ ≳ 10¹⁰ M☉ ) have significantly higher BHAR/SFR ratios than less massive galaxies, indicating that the former have higher SMBH fueling efficiency and/or higher SMBH occupation fraction than the latter. Our results can naturally explain the observed proportionality between MBH and M* for local giant ellipticals and suggest that their MBH M* is higher than that of local star-forming galaxies. Among local star-forming galaxies, massive systems might have higher MBH M* compared to dwarfs.

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  • The Astrophysical Journal, 2017. Washington, DC: The American Astronomical Society.

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  • Publication Title: The Astrophysical Journal
  • Volume: 842
  • Issue: 2
  • Page Start: 1
  • Page End: 17
  • Peer Reviewed: Yes

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  • June 15, 2017

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  • Aug. 8, 2018, 8:27 a.m.

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  • March 16, 2021, 11:10 a.m.

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Yang, G.; Chen, C. -T. J.; Vito, F.; Brandt, William Nielsen; Alexander, David M.; Luo, Bin et al. Black Hole Growth Is Mainly Linked to Host-galaxy Stellar Mass Rather Than Star Formation Rate, article, June 15, 2017; Washington, DC. (https://digital.library.unt.edu/ark:/67531/metadc1225782/: accessed March 31, 2023), University of North Texas Libraries, UNT Digital Library, https://digital.library.unt.edu; crediting UNT College of Science.

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