Accretion and star formation rates in low‐redshift type II active galactic nuclei
By H. Netzer. 2009
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Accretion and star formation (SF) rates in low-redshift Sloan Digital Sky Survey type II active galactic nuclei (AGN) are critically evaluated. Comparison with photoionization models indicates that bolometric luminosity (L bol ) estimates based on L([O III] λ5007) severely underestimate L bol in low-ionization sources such as LINERs. An alternative method based on L(Hβ) is less sensitive to the ionization level, and a novel method, based on a combination of L([O III] λ5007) and L([O I] λ6300), is perhaps the best. Using this method, I show that low-ionization AGN are accreting faster than assumed until now. Other significant related findings are as follows. (1) Any type II AGN property related to the black hole (BH) mass is more reliably obtained by removing blue galaxies from the sample. (2) Seyfert 2s and LINER 2s form a continuous sequence of L/L Edd with no indication for a change in accretion mechanism or mode of mass supply. There are very few, if any, LINERs in all type I samples which results in a much narrower L/L Edd distribution compared with type II samples. (3) There is a strong correlation between the SF luminosity, L SF , and L bol over more than five orders of magnitude in luminosity. This leads to a simple relationship between bulge and BH growth rates, g( bul g e )/g(BH ) ∝ L -0.2 bol , where g( bulge )/g(BH) = 115 for L bol = 10 42 erg s -1 . Seyfert 2s and LINER 2s follow the same L SF -L bol correlation for all sources with a stellar age indicator, D n 4000, smaller than 1.8. This suggests that a similar fraction of SF gas finds its way to the centre in all AGN. (4) L bol , L sF , L/L Edd and the specific SF rate follow D n 4000 in a similar way.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/88dd913f61da04648d3c81e6e9366ab73500c9e7
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Citations in the corpus
- Revisiting the Unified Model of Active Galactic Nuclei (2015, background): “The line is not a very good luminosity indicator in low ionization AGNs like LINERs (Netzer 2009) and it is now known that L([O iii]λ5007)/LAGN is changing with LAGN (Stern & Laor 2012).”
- AGN wind scaling relations and the co-evolution of black holes and galaxies (2017, methodology): “3, right panel, the expected SFR based on the SFR−Lbol correlations by Netzer (2009), Hickox et al. (2014), z = 0, and Hickox et al. (2014), z = 2.”
- A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties (2023, methodology): “As the upper limit, we use the following equation in Netzer (2009) where the H β luminosity is estimated from the extinction-corrected narrow-line H α line assuming Case B recombination.”
- The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, methodology): “However, when taking the suite of models as a whole, it is clear that much time is indeed spent near the ‘correlation line’ from Netzer (2009) and§4.1, mostly when star formation and accretion decay after the merger.”
- Hot graphite dust and the infrared spectral energy distribution of active galactic nuclei (2011, methodology): “We also show theLSF = Lbol line and the relationshipLSF = 1043× ( Lbol/1043 )0.7 ergs−1 which is adopted from the correlation shown in Netzer (2009).”
- Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschel observations (2012, methodology): “This circumstance is suggested by several models (e.g. Di Matteo et al. 2005; Hopkins et al. 2006; Netzer 2009), which assume that AGNs are fuelled only when substantial amounts of gas can reach the central black holes.”
- Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, background): “…single scenario has not yet been derived, it is currently believed that most luminous AGN (LAGN > 1044 erg s−1) are triggered by major merger events (Netzer 2009; Santini et al. 2012), while their fainter counterparts are fueled through secular processes (Shao et al. 2010; Lutz et al. 2010;…”
- Faint high-redshift AGN in the Chandra deep field south: the evolution of the AGN luminosity function and black hole demography (2011, methodology): “At z 0.3, we used the distribution of Netzer (2009b), which are shifted toward higher Eddington ratios with respect to the Kauffmann & Heckman (2009) distributions (see the discussion in Netzer 2009b,a).”
- Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, background): “…distribution of specific accretion rates (or, for that matter, Eddington ratios) is typically found to be lognormal (e.g. Kollmeier et al. 2006; Netzer 2009; Trakhtenbrot et al. 2011; Lusso et al. 2012), rather than a power law, is because of the combined effects of a flux-limited survey,…”
- BLACK HOLE VARIABILITY AND THE STAR FORMATION–ACTIVE GALACTIC NUCLEUS CONNECTION: DO ALL STAR-FORMING GALAXIES HOST AN ACTIVE GALACTIC NUCLEUS? (2013, methodology): “Thus there emerges a strong correlation between 〈LIR〉 and LAGN, as observed in a number of studies (e.g., Lutz et al. 2008; Netzer 2009; Bonfield et al. 2011).”
- The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “Although LINERs typically have lower nuclear luminosities than Seyferts, many of the fundamental characteristics of the objects close to the demarcation boundary are very similar to those of the low-luminosity end of the distribution of Seyferts (e.g. Kewley et al. 2006, Ho 2008, Netzer 2009).”