Dusty, Radiation Pressure-Dominated Photoionization. II. Multiwavelength Emission Line Diagnostics for Narrow-Line Regions

By B. Groves, M. Dopita, R. Sutherland. 2004

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Seyfert narrow-line region (NLR) emission line ratios are remarkably uniform, displaying only ∼0.5 dex variation between galaxies, and even less within an individual object. Previous photoionization and shock models of this region were unable to explain this observation without the introduction of arbitrary assumptions or additional parameters. Dusty, radiation pressure-dominated photoionization models provide a simple physical mechanism that can reproduce this spectral uniformity between different objects. In the first paper of this series, we described this model and its implementation in detail, as well as presenting grids of model emission lines and examining the model structures. Here we explore these models further, demonstrating their ability to reproduce the observed Seyfert line ratios on standard line diagnostic diagrams in both the optical and UV. We also investigate the effects that the variation of metallicity, density, and ionizing spectrum have upon both the new paradigm and the standard photoionization models used hitherto. Along with the standard diagnostic diagrams we provide several new diagnostic diagrams in the UV, optical, and IR. These new diagrams can provide further tests of the dusty, radiation pressure photoionization paradigm as well as being used as diagnostics of the metallicity, density, and ionizing spectrum of the emission line clouds.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1308fe3e12d548ac4955bea1637b9f59487cb089

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Citations in the corpus

Nuclear activity versus star formation: emission-line diagnostics at ultraviolet and optical wavelengths (2015, methodology): “Secondary production of nitrogen is accounted for following the prescription of Groves et al. (2004a), [N/H] = [O/H] ( 10−1.6 + 10(2.33+log10 [O/H]) ) .”
A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, background): “On the other hand it does not guarantee the exclusion of other sources of non stellar ionization that can populate this area, such as shocks (e.g., Allen et al. 2008; Levesque et al. 2010), postAGB stars (e.g., Kehrig et al. 2012), and dusty AGNs (e.g., Groves et al. 2004).”
SDSS IV MaNGA – spatially resolved diagnostic diagrams: a proof that many galaxies are LIERs (2016, background): “A variety of models have been proposed to explain these observations, the most successful of which are dusty radiation pressure-dominated AGN models (Dopita et al. 2002; Groves et al. 2004a,b).”
THE MASS–METALLICITY RELATION WITH THE DIRECT METHOD ON STACKED SPECTRA OF SDSS GALAXIES (2012, methodology): “Theoretical calibrations are based on stellar population synthesis models, like STARBURST99 (Leitherer et al. 1999), and photoionization models, such as MAPPINGS (Sutherland & Dopita 1993; Groves et al. 2004a, 2004b) and CLOUDY (Ferland et al. 1998).”
Distant radio galaxies and their environments (2008, background): “…1 = Miley (1980), 2 = Klamer et al (2006), 3 = Felten and Morrison (1966), 4 = Schwartz (2002), 5 = Osterbrock and Ferland (2006), 6 = Groves et al (2004), 7 = Groves et al (2004), 8 = Dopita and Sutherland (2003), 9 = Aller (1984), 10 = Dickson et al (1995), 11 = Morganti (2006), 12…”
OUTFLOWS FROM ACTIVE GALACTIC NUCLEI: KINEMATICS OF THE NARROW-LINE AND CORONAL-LINE REGIONS IN SEYFERT GALAXIES, (2011, background): “Recently, studies have shown that most of the emission lines seen in the NLR and CLR can be accounted for by assuming a central ionization source illuminating a multicomponent gas (Kraemer et al. 2000; Groves et al. 2004; Mullaney et al. 2009; Mazzalay et al. 2010).”
On the Origin of [O II] Emission in Red-Sequence and Poststarburst Galaxies (2005, methodology): “Besides photoionization by a central nonstellar source, such as an accretion-powered system (Ferland &Netzer 1983; Halpern& Steiner 1983; Groves et al. 2004b), many ionization mechanisms have been proposed to explain the LINER- and TO-like optical emission in early-type galaxies: (1)…”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “2002; Groves et al. 2004a, for a description of the influence of these effects on nebular emission).”
Accretion and star formation rates in low‐redshift type II active galactic nuclei (2009, methodology): “The differences are attributed to changes in the ionization parameter of the line emitting gas (e.g. Ferland and Netzer 1983; Netzer 1990; Groves et al 2004).”
The host galaxies and classification of active galactic nuclei (2006, methodology): “Assuming a bolometric correction of LBOL = 3500L[OIII]o (Heckman et al. 2004) where L[O iii]o is the observed [O iii] luminosity, and assuming a mean extinction of E(B − V) = 0.3, our SeyfertLINER transition corresponds to an Eddington ratio of L/LEDD ∼ 0.05.”