A Theoretical Recalibration of the Extragalactic H II Region Sequence

By M. Dopita, Lisa J. Kewley, C. Heisler, R. Sutherland. 2000

239 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/234a2a6132158e470974f48656f34f586028d17a

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In Astronomy and Astrophysics

Citations in the corpus

Using Strong Lines to Estimate Abundances in Extragalactic H II Regions and Starburst Galaxies (2002, methodology): “These data have the additional advantage of covering a large range in metallicity and ionization parameter, as was shown in Dopita et al. (2000).”
Galaxy pairs in the Sloan Digital Sky Survey - IV: Interactions trigger AGN (2011, background): “…Veilleux & Osterbrock1987), line ratio diagrams have evolved into a standard tool for categorizing the dominant source of ionizing radiation in a galaxy (Dopita et al. 2000; Kewley et al. 2001, 2006b; Kauffmann et al. 2003a; Stasinska et al. 2006; Groves et al. 2006; Cid-Fernandes et al. 2010).”
[O II] as a Star Formation Rate Indicator (2004, methodology): “The C01 case F diagnostic is potentially problematic for our sample because the [O iii]/H ratio is relatively insensitive to metallicity (e.g., Dopita et al. 2000).”
Metallicity and Nuclear Star Formation in Nearby Galaxy Pairs: Evidence for Tidally Induced Gas Flows (2005, methodology): “These models successfully reproduce the H II region abundance sequence (Dopita et al. 2000), the abundance sequence of star-forming galaxies (Kewley et al. 2001a), and individual star clusters within galaxies (Calzetti et al. 2004).”
Realistic ionizing fluxes for young stellar populations from 0.05 to 2 Z (2002, methodology): “We adopt the abundances and depletion factors given by Dopita et al. (2000) for solar metallicity and scale these for other metallicities.”
Nebular Continuum and Line Emission in Stellar Population Synthesis Models (2016, methodology): “N2O2: The [N II] λ6548/[O II] λ3727 (N2O2) line ratio correlates with metallicity and is widely used as an abundance indicator (Veilleux & Osterbrock 1987; Dopita et al. 2000; Levesque et al. 2010).”
Inferring the star formation histories of massive quiescent galaxies with bagpipes: evidence for multiple quenching mechanisms (2017, methodology): “We assume the metallicity of the ionized gas is the same as the stars which produce the ionizing photons and use the Solar abundances of Anders & Grevesse (1989) and ISM depletion factors and Helium and Nitrogen scaling relations of Dopita et al. (2000).”
Metallicities and Physical Conditions in Star-forming Galaxies at z ~ 1.0-1.5 (2008, methodology): “…spectrum in an H II region, i.e., the gas phase metallicity, the shape or hardness of theion- izing radiation spectrum, and the geometrical distribution of gas with respect to the ionizing sources, which can be represented by the mean ionization parameter and electron density (Dopita et al. 2000).”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, background): “In practice, all models with a similar effective ionization parameter 4 produce very similar spectra, assuming all other parameters are held constant (e.g., Dopita et al. 2000).”
OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, methodology): “…in which various nebular emission-line ratios are tracked as a function of the input metallicity and ionization parameter (McGaugh 1991; Dopita et al. 2000, 2006a; Charlot & Longhetti 2001; Kewley & Dopita 2002).18 Among published strong-line calibrations there exist large, poorly…”
Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies (2014, background): “The location on the BPT diagram has a complex dependence on parameters like metallicity, ionization, age and temperature (e.g. Dopita et al. 2000, 2006; Pérez-Montero & Dı́az 2005; Levesque, Kewley & Larson 2010b; Steidel et al. 2014; Sánchez et al. 2015).”
Chemical Abundances of DEEP2 Star-forming Galaxies at z~1.0-1.5 (2005, methodology): “The starbursts in the Kewley et al. (2001b) sample not accounted for by the upper envelope of the H II region emission-line sequence of Dopita et al. (2000) are found in a similar location to the DEEP2 z ∼ 1.4 galaxies, in [OIII]/Hβ vs. [NII]/Hα parameter space.”
Optical Star Formation Rate Indicators (2005, unknown): “The observed differences are consistent with the higher mean luminosity and metallicity of the SDSS galaxies (Dopita et al. 2000; Kewley et al. 2001a), and with the inclusion of a larger number of extreme starbursts with hard ionizing radiation fields in the integrated galaxy sample.”
GALEX–SDSS–WISE LEGACY CATALOG (GSWLC): STAR FORMATION RATES, STELLAR MASSES, AND DUST ATTENUATIONS OF 700,000 LOW-REDSHIFT GALAXIES (2016, background): “We select the lowest ionization parameter available, log U = −3, as it produces the biggest improvements and is closest to direct measurements (Dopita et al. 2000; Liang et al. 2006).”
GALAXY-WIDE SHOCKS IN LATE-MERGER STAGE LUMINOUS INFRARED GALAXIES (2011, background): “The primary factors influencing emission line strengths are the shape of the extreme ultraviolet (EUV) spectrum and the abundance of the emission line gas (Kewley et al. 2001; Dopita et al. 2000).”
Active Galactic Nuclei in the Sloan Digital Sky Survey. I. Sample Selection (2005, background): “The cause could again be shock excitation: the relatively cool high-density regions formed behind the shock front emit strong [S ii] emission lines (Dopita et al. 2000).”
Ionization state of inter-stellar medium in galaxies: evolution, SFR-M * -Z dependence, and ionizing photon escape (2013, background): “MNRAS 442, 900–916 (2014) Downloaded from https://academic.oup.com/mnras/article-abstract/442/1/900/1252695 by guest on 28 July 2018 ing of O2 + is more efficient than those in optical wavelength (e.g. Dopita et al. 2000; Charlot & Longhetti 2001).”