Oxygen Abundance Determination in H II Regions: The Strong Line Intensities-Abundance Calibration Revisited

By L. Pilyugin, T. Thuan. 2005

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In Astronomy and Astrophysics

Citations in the corpus

Metallicity Calibrations and the Mass-Metallicity Relation for Star-forming Galaxies (2008, methodology): “…calibrations are based on the optical line ratios [N II] λ6584/Hα (Pettini & Pagel 2004), ([O III]/Hβ)/([N II]/Hα), (Pettini & Pagel 2004, ; hereafter PP04), or the “R23” ratio (([O II] λ3727 +[O III] λλ4959,5007)/Hβ (Pilyugin 2001; Pilyugin & Thuan 2005; Liang et al. 2007; Yin et al. 2007b)).”
EXTRAGALACTIC CHEMICAL ABUNDANCES: DO H ii REGIONS AND YOUNG STARS TELL THE SAME STORY? THE CASE OF THE SPIRAL GALAXY NGC 300 (2009, background): “Empirical calibrations that are tied to auroral line measurements (such as those by Pettini & Pagel 2004, Pilyugin & Thuan 2005 and Liang et al. 2007) provide considerably smaller abundance values (0.2-0.6 dex) than theoretical calibrations, which are generated from grids of photoionization models…”
The Herschel Dwarf Galaxy Survey - I. Properties of the low-metallicity ISM from PACS spectroscopy (2015, methodology): “In the SINGS galaxies, it is 12 + log(O/H) = 8.4 with the Pilyugin & Thuan (2005) calibration and 12+ log(O/H) = 9.0 with the Kobulnicky & Kewley (2004) calibration (Moustakas et al. 2010), with larger discrepancies in the methods for massive galaxies (Kewley & Ellison 2008).”
RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, methodology): “These authors compute the oxygen abundances using two different calibrations: Kobulnicky & Kewley (2004) and Pilyugin & Thuan (2005).”
An Overview of the Dwarf Galaxy Survey (2013, methodology): “In order to ensure homogeneity in the calibration of the metallicity values in the DGS sample, metallicities were recomputed from optical line intensities following the methods of Izotov et al. (2006) (I06) and Pilyugin & Thuan (2005) (PT05) and compared.”
New fully empirical calibrations of strong-line metallicity indicators in star forming galaxies (2016, methodology): “…can be obtained either empirically, for samples in which metallicity have been previously derived with the Te method (e.g. Pettini & Pagel 2004; Pilyugin & Thuan 2005; Pilyugin et al. 2010b, 2012; Marino et al. 2013; Pilyugin & Grebel 2016), or theoretically, in which oxygen abundance have…”
Eliminating error in the chemical abundance scale for extragalactic H ii regions (2012, methodology): “Subsequently, Pilyugin & Thuan (2005) and Pilyugin, Vı́lchez & Thuan (2010) tried to improved such calibrations including more spectroscopic measurements of H ii regions in spiral and irregular galaxies derived using the Te-method.”
THE MOSDEF SURVEY: MASS, METALLICITY, AND STAR-FORMATION RATE AT z ∼ 2.3 (2014, background): “…can be calibrated to “direct” electron temperature-determined metallicities from measuring auroral lines such as [O iii]λ4363 (Pettini & Pagel 2004; Pilyugin & Thuan 2005) or photoionization models of star-forming regions (Zaritsky et al. 1994; Kewley & Dopita 2002; Kobulnicky & Kewley 2004;…”
Probing the dust properties of galaxies up to submillimetre wavelengths. II. Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf galaxies (2011, methodology): “For M51, Moustakas & Kennicutt (2006) also estimated the metallicity to be 12 + log(O/H) = 8.7 using Pilyugin & Thuan (2005) but their estimate reaches 9.2 using the McGaugh (1991) strong-line calibration of the R23.”
THE EMISSION BY DUST AND STARS OF NEARBY GALAXIES IN THE HERSCHEL KINGFISH SURVEY (2011, methodology): “The absolute metallicity scales we use to split the sample are 12 + log (O/H) = 8.88 and 9.08 (or 8.29 and 8.42 using the Pilyugin & Thuan (2005) calibration), but these absolute abundances should be treated with caution.”
The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, methodology): “An overview of the spectroscopy 1 Oxygen abundances, which are used here to constrain metallicities, are calculated from optical line intensities following the prescriptions in Pilyugin & Thuan (2005), assuming a solar oxygen abundance O/H = 4.9 × 10−4, or 12 + log (O/H) = 8.7 (Asplund et al. 2009).”
The assembly of ‘normal’ galaxies at z ∼ 7 probed by ALMA (2015, methodology): “ALMA observations of normal galaxies at z∼7 11 priv. comm.) and from Moustakas et al. (2010) (in the latter we have used the calibrations from Pilyugin & Thuan 2005).”
DIRECT OXYGEN ABUNDANCES FOR LOW-LUMINOSITY LVL GALAXIES (2012, methodology): “Because of the possibility that these objects’ oxygen abundances were underestimated using the lower branch of the R23 calibration (Pilyugin & Thuan 2005), they were included in this sample to be re-examined (see discussion in Appendix B).”
New calibrations for abundance determinations in H ii regions (2016, methodology): “This diagram was used to construct calibrations for oxygen abundance determinations by numerous investigators (e.g., Edmunds & Pagel 1984; Dopita & Evans 1986; McGaugh 1991; Zaritsky, Kennicutt & Huchra 1994; Pilyugin 2000, 2001a; Pilyugin & Thuan 2005).”
A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, methodology): “Recently, Bresolin (2011) has redetermined the abundance gradient of NGC 4258 by adopting the Pilyugin & Thuan (2005) calibration of R23.”
The role of cold gas and environment on the stellar mass-metallicity relation of nearby galaxies (2012, methodology): “…lines, such as [Oiii] λ3727, [Oiii] λ4959, [Oiii] λ5007 and Hβ in the R23 method (e.g. Pagel et al. 1979; McGaugh 1991; Kobulnicky & Kewley 2004; Pilyugin & Thuan 2005), the [Nii] λ6584/Hα ratio (e.g. Denicoló et al. 2002; Pettini & Pagel 2004) and the [Nii] λ6584/[Oii] λ3727 ratio (Kewley…”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, neutral): “J.Moustakas et al. (2007, in preparation) show that different ‘‘strongline’’ methods (e.g., Kobulnicky & Kewley 2004 vs. Pilyugin & Thuan 2005) give differing estimates for (O/H), with the Pilyugin & Thuan (2005) values tending to be smaller than the Kobulnicky & Kewley (2004) values by a factor of…”