Dusty, Radiation Pressure-Dominated Photoionization. I. Model Description, Structure, and Grids

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

244 citations recorded by the source corpus.

We present the implementation of dusty, radiation pressure-dominated photoionization models applicable to the narrow-line regions (NLRs) of active galactic nuclei, using the MAPPINGS III code. We give a grid of the predicted intensities of the most commonly used diagnostic spectral lines in the UV, optical, and IR, covering a wide range of density, metallicity, the power-law index characterizing the photoionizing source, and photoionization parameter, for use in the diagnosis of NLRs. We examine the temperature, density, and ionization structure of these models, investigating the effect of variation of these parameters in order to gain a better understanding of NLR clouds themselves.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/cee0b829b18e994ef18192e185916ebb64d1cb98

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Citations in the corpus

Emission-line diagnostics of low-metallicity active galactic nuclei (2006, methodology): “As discussed in Groves et al. (2004a), the abundance with respect to hydrogen of most of the elements listed in table 1 will scale linearly with total metallicity.”
Nebular Continuum and Line Emission in Stellar Population Synthesis Models (2016, background): “Popular photoionization codes include CLOUDY (Ferland et al. 2013) and MAPPINGS-III (Groves et al. 2004), both of which compute the full radiative transfer through a gas cloud and predict the resultant emission spectrum.”
A New Sample of Low-Mass Black Holes in Active Galaxies (2007, background): “On the other hand, changes in ionization parameter move, for example, [NII ]/Hα vs. [O III ]/Hβ on tracks perpendicular to those observed (e.g., Groves et al. 2004a,b).”
GALAXY ZOO: THE FUNDAMENTALLY DIFFERENT CO-EVOLUTION OF SUPERMASSIVE BLACK HOLES AND THEIR EARLY- AND LATE-TYPE HOST GALAXIES (2010, unknown): “…by many theorists using photoionisation codes (e.g., Stasińska 1990; Leitherer & Heckman 1995; Leitherer et al. 1999; Kewley et al. 2001, 2006; Groves et al. 2004a,b) and by observational work (e.g., Veilleux & Osterbrock 1987; Ho et al. 1995, 1997a,b,c; Kauffmann et al. 2003a; Stasińska et…”
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).”
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)…”
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]) ) .”
OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, background): “…young stars, including the effects of mass loss and rotation (Vázquez & Leitherer 2005), the calculation of non-LTE, line-blanketed stellar atmospheres (Simón-Dı́az & Stasińska 2008), and the inclusion of dust grains in the photoionization models (Shields & Kennicutt 1995; Groves et al. 2004).”
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).”
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).”
Metallicity Calibrations and the Mass-Metallicity Relation for Star-forming Galaxies (2008, methodology): “Current state-of-the-art photoionization models such as MAPPINGS (Sutherland & Dopita 1993; Groves et al. 2004, 2006) and CLOUDY (Ferland et al. 1998) calculate the thermal balance at steps through a dusty spherical or plane parallel nebula.”
The MAPPINGS III Library of Fast Radiative Shock Models (2008, methodology): “This choice ALLEN ET AL.50 of metallicity is driven by thework of Groves et al. (2004a, 2006), who find that supersolar metallicity photoionization models best reproduce the observed narrow-line ratios in AGNs, and the work of Kauffmann et al. (2003), who find that AGNs are typically hosted in…”
Dusty, Radiation Pressure-Dominated Photoionization. II. Multiwavelength Emission Line Diagnostics for Narrow-Line Regions (2004, methodology): “We described the implementation of these models in depth in Paper I of this series (Groves et al. 2004), where we gave the emission line strengths from these models in a sequence of tables covering the parameter space.”
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…”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, methodology): “We use the Mappings III dusty, radiation pressure dominated models of Groves et al. (2004a).”