ner_tags: B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O B-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation O O O B-Model I-Model I-Model B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation O B-Citation I-Citation I-Citation I-Citation B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O B-CelestialObject I-CelestialObject O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation O B-Citation I-Citation I-Citation
tokens: Hirschmann et al. 2010 ; Jahnke Macciò 2011 ). A closely related issue involves the connection between BH accretion and star formation in the host galaxy. Here, too, no consensus has yet emerged. While some contend that star formation rate (SFR) correlates strongly with AGN luminosity across a wide range of redshifts, implying the simultaneous growth of the BH and its host (e.g., Bonfield et al. 2011 ; Rosario et al. 2012 ; Xu et al. 2015 ; Lanzuisi et al. 2017 ; Dai et al. 2018 ; Stemo et al. 2020 ), others find only moderate or no correlation (Rosario et al. 2013 ; Azadi et al. 2015 ; Stanley et al. 2015 , 2017 ). The disagreement is partly explained by the different timescales of the measured SFR and AGN variability (Hickox et al. 2014 ). At high redshifts (e.g., z > 1), many works do not find a significant correlation between SFR and AGN luminosity (e.g., Shao et al. 2010 ; Rosario et al. 2012 ; Schulze et al. 2019 ; but see Stemo et al. 2020 ). For low redshifts, the correlation is moderate in weak AGNs (e.g., Shimizu et al. 2017 ) but strong in more powerful systems (e.g., Netzer 2009 ; Imanishi et al. 2011 ; Xia et al. 2012 ; Lani et al. 2017 ; Zhuang Ho 2020 ). It has also been argued that the relationship between SFR and AGN luminosity is not intrinsic but instead arises indirectly from the the mutual correlation of both quantities to the host galaxy stellar mass (e.g., Xu et al. 2015 ; Yang et al. 2017 ; Suh et al. 2019 ; Stemo et al. 2020 ), stellar mass surface density (Ni et al. 2020 ), or BH mass (e.g., Stanley et al. 2017 ). Using a hierarchical Bayesian model, Grimmett et al. ( 2020 ) recently demonstrated that AGNs of higher X-ray luminosity more tightly correlate with higher SFRs than lower luminosity AGNs. In any event, when present, the association between star formation and BH accretion seems to occur preferentially on nuclear scales, both in moderately luminous AGNs (Davies et al. 2007 ; Watabe et al. 2008 ; Diamond-Stanic Rieke 2012 ; Esquej et al. 2014 ; Zhuang Ho 2020 ) and in more powerful quasars (Imanishi et al. 2011 ; Canalizo Stockton 2013 ; Bessiere et al. 2014 , 2017 ; Lutz et al. 2016; Kim Ho 2019 ; Zhao et al. 2019 ). This is not unexpected, as cold gas on small scales naturally fuels nuclear star formation and feeds the BH (Hopkins Quataert 2010 ; Volonteri et al. 2015 ; Gan et al. 2019 ). Observations of nearby galactic nuclei offer useful clues. For example, the molecular gas in the central regions of many galaxies (e.g., Scoville et al. 1994 ; Smith Harvey 1996 ; Rubin et al. 1997 ; García-Burillo et al. 2005 , 2019 ; Hicks et al. 2009 ; Izumi et al. 2018 ; Salak et al. 2018 ; Treister et al. 2018 ; Boizelle et al. 2019 ), including the Milky Way (e.g., Ho et al. 1991 ; Hsieh et al. 2017 ), resides in the form of a circumnuclear disk. Theoretical works suggest that the star formation in the circumnuclear disk may control the gas fueling BH accretion (Shlosman et al. 1989 ; Goodman 2003 ; Thompson et al.