On the oxygen abundance determination in HII regions. - High-metallicity regions

By L. Pilyugin. 2001

199 citations recorded by the source corpus.

This is our second paper devoted to the problem of line intensity -oxygen abundance calibration starting from the idea of McGaugh ([CITE]) that the strong oxygen lines ($[{\rm OII}] \lambda \lambda 3727, 3729$ and $[{\rm OIII}] \lambda \lambda 4959, 5007$) contain the necessary information to determine accurate abundances in HII regions. In the previous study (Pilyugin 2000) the corresponding relations were obtained for the low-metallicity HII regions ($12+{\rm log O/H} \leq 7.95$, the lower branch of the O/H - R 23 diagram). The high-metallicity HII regions ($12+{\rm log O/H} \geq 8.2$, the upper branch of the O/H - R 23 diagram) are considered in the present study. A relation of the type ${\rm O/H}=f(P, R_{23}$) between oxygen abundance and the value of abundance index R 23 , introduced by Pagel et al. ([CITE]), and the excitation parameter P (which is defined here as the contribution of the radiation in $[{\rm OIII}] \lambda \lambda 4959, 5007$ lines to the "total" oxygen radiation) has been derived empirically using the available oxygen abundances determined via measurement of a temperature-sensitive line ratio [OIII]4959,5007/[OIII]4363 ( T e -method). By comparing oxygen abundances in high-metallicity HII regions derived with the T e -method and those derived with the suggested relations ( P -method), it was found that the precision of oxygen abundance determination with the P -method is around 0.1 dex (the mean difference for the 38 HII regions considered is ~0.08 dex) and is comparable to that of the T e -method. A relation of the type $T_{\rm e}=f(P, R_{23}$) between electron temperature and the values of abundance index R 23 and the excitation parameter P was derived empirically using the available electron temperatures determined via measurement of temperature-sensitive line ratios. The maximum value of differences between electron temperatures determined via measurement of temperature-sensitive line ratios and those derived with the suggested relation is around 1000 K for HII regions considered here, the mean value of differences for 38 HII regions is ~500 K, which is the same order of magnitude as the uncertainties of electron temperature determinations in high-metallicity HII regions via measured temperature-sensitive line ratios.

Subfields: Aerospace Engineering, Mechanics of Materials, Radiation

View Paper: https://www.semanticscholar.org/paper/cb8fa0e332126afc94791a62ccde24ae6d04dacd

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Citations in the corpus

Measuring Global Galaxy Metallicities Using Emission-Line Equivalent Widths (2003, unknown): “The translation of these errors into errors in oxygen abundance will depend on the value of R 23 , but for the upper-metallicity branch away from the “turnaround” point, the slope of log(O/H) vs log( R 23 ) is ∼ 1.4 (Pilyugin 2001), so the addition error in log(O/H) would be ∼ 0.11 dex.”
Oxygen Abundance Determination in H II Regions: The Strong Line Intensities-Abundance Calibration Revisited (2005, methodology): “…McGaugh (1991) that the strong oxygen lines may contain the necessary information to determine the oxygen abundance in low-metallicity H ii regions, Pilyugin (2000, 2001a, 2001b) has shown that the physical conditions in an H ii region can be estimated and taken into account via the excitation…”
The Metallicity of Galaxy Disks: Infall versus Outflow (2006, methodology): “…in Pilyugin et al. (2004) were calculated using gas-phase oxygen abundances measured from HII region spectroscopy using the “P -method”, developed in Pilyugin (2000, 2001a) to match accurate oxygen abundances based on temperature-sensitive line ratios involving the weak [OIII]λ4363 line…”
NEW STRONG-LINE ABUNDANCE DIAGNOSTICS FOR H ii REGIONS: EFFECTS OF κ-DISTRIBUTED ELECTRON ENERGIES AND NEW ATOMIC DATA (2013, methodology): “…1991; Kewley & Dopita 2002; Kobulnicky & Kewley 2004) and those based upon an empirical alignment of the strong line intensities to abundances derived in objects for which Te has been directly estimated (Pilyugin 2001a, 2001b; Bresolin et al. 2004; Pilyugin & Thuan 2005; Pilyugin et al. 2012).”
Eliminating error in the chemical abundance scale for extragalactic H ii regions (2012, methodology): “His first empirical calibrations involving both the R23 and the P parameter were presented in Pilyugin (2001a) and Pilyugin (2001b) for high- and low-metallicity H ii regions.”
Using Strong Lines to Estimate Abundances in Extragalactic H II Regions and Starburst Galaxies (2002, background): “Examples include Alloin et al. (1979), Edmunds & Pagel (1984), McCall et al. (1985), Dopita & Evans (1986), Pilyugin (2000, 2001), McGaugh (1991), and Charlot & Longhetti (2001).”
The luminosity–metallicity relation in the local Universe from the 2dF Galaxy Redshift Survey (2004, methodology): “…through the parameterR 23 introduced initially by Pagel et al. (1979), and defined as follow: c 2004 RAS, MNRAS000, 1–11 R 23 = [O III] 4959;5007+ [O II] 3727 H (4) Extensive studies have been dedicated to calibrate the relation betweenR 23 and oxygen abundance (McCall et al. 1985; Pilyugin 2001b).”
OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, methodology): “(A color version of this figure is available in the online journal.) is an excitation parameter (Pilyugin 2001) that is analogous to Equation (4) for the KK04 calibration.”
New calibrations for abundance determinations in H ii regions (2016, methodology): “…the emission lines of different elements were suggested (Edmunds & Pagel 1984; Dopita & Evans 1986; McGaugh 1991; Zaritsky, Kennicutt & Huchra 1994; Pilyugin 2000, 2001a; Kewley & Dopita 2002; Pettini & Pagel 2004; Tremonti et al. 2004; Pilyugin & Thuan 2005; Stası́nska 2006; Pilyugin et al. 2010;…”
Optical Star Formation Rate Indicators (2005, unknown): “In addition, R23 depends on the ionization parameter, particularly at low metallicity (e.g., Kobulnicky et al. 1999), and possibly even at high metallicity (Pilyugin 2001).”
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, methodology): “=([O ii] λ3727+[O iii] λ4959+[O iii] λ5007)/Hβ is a commonly used metallicity indicator (McGaugh 1991; Zaritsky et al. 1994; Pilyugin 2001; Kewley & Dopita 2002; Kobulnicky & Kewley 2004).”
Abundances of Metal-rich H II Regions in M51 (2004, methodology): “In this plot, only objects which are predicted by the P-method to have 12 + log (O/H)>8.2 (the quoted range of validity for this method in the high-abundance regime) are plotted.”
A VLT study of metal-rich extragalactic H II regions - I. Observations and empirical abundances (2005, methodology): “The Pilyugin (2001) calibration attempts to account for the sensitivity of R23 to the ionization parameter, by introducing the quantity P= [O ] λλ4959,5007/([O ] λ3727+ [O ] λλ4959,5007).”
The Composition Gradient in M101 Revisited. II. Electron Temperatures and Implications for the Nebular Abundance Scale (2003, methodology): “Figure 14 shows a comparison of direct abundances with empirical values derived using the ‘‘P method ’’ of Pilyugin (2001a).”