The Mass–Metallicity Relation of Local Active Galaxies

Childress, M.; Kewley, Lisa J.; Dopita, Michael A.; Groves, Brent; Hopkins, A. M.; Sutherland, Ralph S.

doi:10.3847/1538-4357/ab08a1

Cited by 46 publications

(59 citation statements)

References 63 publications

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“…0, 8.40, 8,56, 8.69, 8.86, 9.00, respectively, Metallicity values in this range has been found for AGNs with redshifts varying from ∼ 0 to ∼ 7 (e.g. Nagao et al 2006a;Feltre, Charlot & Gutkin 2016;Matsuoka et al 2018;Thomas et al 2019;Mignoli et al 2019;Pérez-Montero et al 2019;Dors et al 2014Dors et al , 2015Dors et al , 2018. We found that photoionization models assuming (Z/Z⊙) > 2.0 produce similar intensities of N 2, therefore, only (Z/Z⊙) < = 2.0 were assumed in our analysis.…”

Section: Photoionization Modelsmentioning

confidence: 86%

Chemical abundances of Seyfert 2 AGNs – II. N2 metallicity calibration based on SDSS

Carvalho

Dors

Cardaci

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a semi-empirical calibration between the metallicity (Z) of Seyfert 2 Active Galactic Nuclei and the N 2=log([N ii]λ6584/Hα) emission-line intensity ratio. This calibration was derived through the [O iii]λ5007/[O ii]λ3727 versus N 2 diagram containing observational data and photoionization model results obtained with the Cloudy code. The observational sample consists of 463 confirmed Seyfert 2 nuclei (redshift z 0.4) taken from the Sloan Digital Sky Survey DR7 dataset. The obtained Z-N 2 relation is valid for the range 0.3 (Z/Z ⊙ ) 2.0 which corresponds to −0.7 (N 2) 0.6. The effects of varying the ionization parameter (U ), electron density and the slope of the spectral energy distribution on the Z estimations are of the order of the uncertainty produced by the error measurements of N 2. This result indicates the large reliability of our Z − N 2 calibration. A relation between U and the [O iii]/[O ii] line ratio, almost independent of other nebular parameter, was obtained.

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Section: Photoionization Modelsmentioning

confidence: 86%

Chemical abundances of Seyfert 2 AGNs – II. N2 metallicity calibration based on SDSS

Carvalho

Dors

Cardaci

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Looking from another perspective, Thomas et al (2019) found a systematic positive offset in the oxygen abundances for Seyfert galaxies in comparison to SFGs from the SDSS DR7. They inspect many possible methodological causes that could artificially create this offset.…”

Section: Mass-metallicity Relationmentioning

confidence: 94%

Galaxies hosting an active galactic nucleus: a view from the CALIFA survey

Lacerda

Sánchez

Fernandes

et al. 2020

Monthly Notices of the Royal Astronomical Society

111

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We study the presence of optically-selected Active Galactic Nuclei (AGNs) within a sample of 867 galaxies extracted from the extended Calar-Alto Legacy Integral Field spectroscopy Area (eCALIFA) spanning all morphological classes. We identify 10 Type-I and 24 Type-II AGNs, amounting to ∼ 4 per cent of our sample, similar to the fraction reported by previous explorations in the same redshift range. We compare the integrated properties of the ionized and molecular gas, and stellar population of AGN hosts and their non-active counterparts, combining them with morphological information. The AGN hosts are found in transitory parts (i.e. green-valley) in almost all analysed properties which present bimodal distributions (i.e. a region where reside star-forming galaxies and another with quiescent/retired ones). Regarding morphology, we find AGN hosts among the most massive galaxies, with enhanced central stellarmass surface density in comparison to the average population at each morphological type. Moreover, their distribution peaks at the Sab-Sb classes and none are found among very late-type galaxies (> Scd). Finally, we inspect how the AGN could act in their hosts regarding the quenching of star-formation. The main role of the AGN in the quenching process appears to be the removal (or heating) of molecular gas, rather than an additional suppression of the already observed decrease of the star-formation efficiency from late-to-early type galaxies.

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“…Our models predict a narrow range (see above) of O/H abundances and the large majority of our sample objects (∼ 99 per cent) shows 12 + log(O/H) values higher than 8.7 dex. A narrow metallicity range for AGNs, with 12+log(O/H) varying by ∼ 0.1 dex as a function of host galaxy stellar mass over the range 10.1 < ∼ log(M/M⊙) < ∼ 11.3, was also derived by Thomas et al (2019), who used the Bayesian parameter estimation code NebulaBayes. The derived narrow O/H range by the composite models for our sample reflects a stronger dependence of oxygen emission lines on shock parameters (e.g.…”

Section: Diagnostic Diagramsmentioning

confidence: 99%

Chemical abundances of Seyfert 2 AGNs – IV. Composite models calculated by photoionization + shocks

Dors

Contini

Riffel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We build detailed composite models of photoionization and shock ionization based on the suma code to reproduce emission lines emitted from the Narrow Line Regions (NLR) of Seyfert 2 nuclei. The aim of this work is to investigate diagram AGN positions according to shock parameters, shock effects on the gas temperature and ionization structures and derive a semi-empirical abundance calibration based on emission-line ratios little sensitive to the shock presence. The models were used to reproduce optical (3000 < λ(Å) < 7000) emission line intensities of 244 local ($z \: {\lesssim}\: 0.4$) Seyfert 2s, whose observational data were selected from Sloan Digital Sky Survey DR7. Our models suggest that shocks in Seyfert 2 nuclei have velocities in the range of 50-300 $\rm km \: s^{-1}$ and imply a narrower metallicity range ($0.6 \: {\lesssim}\: (Z/Z_{\odot }) \: {\lesssim}\: 1.6$) than those derived using pure photoionization models. Our results indicate that shock velocity in AGNs can not be estimated using standard optical line ratio diagrams, based on integrated spectra. Our models predict a different temperature structure and $\rm O^{+}$/O and $\rm O^{2+}$/O fractional abundances throughout the NLR clouds than those derived from pure photoionization models, mainly in shock-dominated objects. This suggests that, in order to minimize the shock effects, the combination of emission-lines emitted by ions with similar intermediate ionization potential could be good metallicity indicators. Finally, we derive two calibrations between the N/O abundance ratio and the N2O2=log([N ii]λ6584/[O ii]λ3727) and N2=log([N ii]λ6584/Hα) indexes which agree with that derived from pure photoionization models.

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The Mass–Metallicity Relation of Local Active Galaxies

Cited by 46 publications

References 63 publications

Chemical abundances of Seyfert 2 AGNs – II. N2 metallicity calibration based on SDSS

Chemical abundances of Seyfert 2 AGNs – II. N2 metallicity calibration based on SDSS

Galaxies hosting an active galactic nucleus: a view from the CALIFA survey

Chemical abundances of Seyfert 2 AGNs – IV. Composite models calculated by photoionization + shocks

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