The chemical composition of metal-poor emission-line galaxies in the Data Release 3 of the Sloan Digital Sky Survey

By Y. Izotov, G. Stasińska, G. Meynet, N. Guseva, T. Observatory, Kyiv, Ukraine, Luth, O. Meudon, France. and 5 more. 2005

496 citations recorded by the source corpus.

We have re-evaluated empirical expressions for the abundance determination of N, O, Ne, S, Cl, Ar and Fe taking into account the latest atomic data and constructing an appropriate grid of photoionization models with state-of-the art model atmospheres. Using these expressions we have derived heavy element abundances in the ∼310 emission-line galaxies from the Data Release 3 of the Sloan Digital Sky Survey (SDSS) with an observed Hβ flux F(Hβ) > 10 −14 erg s −1 cm −2 and for which the [O iii] λ4363 emission line was detected at least at a 2σ level, allowing abundance determination by direct methods. The oxygen abundance 12 + log O/H of the SDSS galaxies lies in the range from ∼7.1 (Z� /30) to ∼8.5 (0.7 Z� ). The SDSS sample is merged with a sample of 109 blue compact dwarf (BCD) galaxies with high quality spectra, which contains extremely low-metallicity objects. We use the merged sample to study the abundance patterns of low-metallicity emission-line galaxies. We find that extremely metal-poor galaxies (12 + log O/H –1.6, implying that they have a different nature than the subsample of high-redshift damped Lyα systems with log N/ Oo f∼–2.3 and that their ages are larger than 100–300 Myr. We confirm the apparent increase in N/O with decreasing EW(Hβ), already shown in previous studies, and explain it as the signature of gradual nitrogen ejection by massive stars from the most recent starburst.

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Citations in the corpus

Semi‐empirical analysis of Sloan Digital Sky Survey galaxies – III. How to distinguish AGN hosts (2006, methodology): “For nitrogen, we also adopt the following law, also based on the paper by Izotov et al. (2006), using their fig.”
EXTRAGALACTIC CHEMICAL ABUNDANCES: DO H ii REGIONS AND YOUNG STARS TELL THE SAME STORY? THE CASE OF THE SPIRAL GALAXY NGC 300 (2009, methodology): “The models that are relevant for our work are those labeled “high Z" [12 + log(O/H)> 8.2] and “intermediate Z" [7.6< 12 + log(O/H)≤ 8.2] by Izotov et al. (2006), who parameterize the ICFs in terms of the observed O+/O. Fig.”
RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, unknown): “…(see Table 7), which gives Te(OIII) = 12250 ± 600 K. Assuming that Te(OII) = 0.7 Te(OIII) + 3000 (e.g., Campbell et al. 1986; Garnett 1992; Izotov et al. 2006; Pilyugin et al. 2009; hereinafter referred to as the “T2 − T3” relation) and that (O/H) = (O++/H+) + (O+/H+), the…”
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.”
JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators (2023, methodology): “We do not take into account a higher ionization abundance of O 3 + / H + , as we follow the approximation given by Izotov et al. ( 2006 ) and con ﬁ rm no clear presence of the He II λ 4686 emission line in the spectra.”
Strongly star forming galaxies in the local Universe with nebular He iiλ4686 emission (2012, methodology): “For all objects with detected [O III] λ4363 with S/N > 3, we also use the Te method, or direct method, using the fitting formulae provided by Izotov et al. (2006a) to estimate the oxygen abundances.”
De re metallica: the cosmic chemical evolution of galaxies (2018, methodology): “While the auroral lines are routinely observed in local or low redshift, metal-poor, star forming galaxies (Kennicutt et al., 2003; Izotov et al., 2006a,b; Izotov & Thuan, 2007; Izotov et al., 2011, 2012; Kreckel et al., 2015; Haurberg et al., 2015; Amorı́n et al., 2015; Pilyugin et al., 2015;…”
Eliminating error in the chemical abundance scale for extragalactic H ii regions (2012, unknown): “This observational result has been also found by Yin et al (2007), Bresolin et al. (2009), Moustakas et al. (2010) and López-Sánchez et al. (2011); in some objects the differences reach up to 0.6 dex.”
Detection of high Lyman continuum leakage from four low-redshift compact star-forming galaxies (2016, methodology): “We use the emission line intensities (Table 5) and the direct Te-method to derive electron temperatures and electron number densities, ionic and total element abundances in the interstellar medium (ISM) of the galaxies as described in Izotov et al. (2006).”
A new determination of the primordial He abundance using the He i λ10830 Å emission line: cosmological implications (2014, methodology): “We use the ionisation correction factors (ICF s) from Izotov et al. (2006) to correct for unseen stages of ionisation and to derive the total O, N, Ne, S, Cl, Ar, and Fe abundances.”
The history of star-forming galaxies in the Sloan Digital Sky Survey (2007, methodology): “The same applies when using the O/H values obtained by Izotov et al. (2006) from direct methods using the electron temperature derived from [OIII]4363/[OIII]5007.”
THE MASS–METALLICITY RELATION WITH THE DIRECT METHOD ON STACKED SPECTRA OF SDSS GALAXIES (2012, methodology): “The Liang et al. (2007) study relies solely on the [O ii] λλ7320, 7330 auroral lines to measure Te[O ii], which is used to infer Te[O iii] and the O++ abundance by applying the T2–T3 relation and Te[O iii]–(O++/H+) formula from Izotov et al. (2006).”
THE PRIMORDIAL ABUNDANCE OF 4He: EVIDENCE FOR NON-STANDARD BIG BANG NUCLEOSYNTHESIS (2010, methodology): “We attribute such a change to oxygen depletion, and correct the oxygen abundance for it, using the log Ne/O versus oxygen abundance regression line found by Izotov et al. (2006), and assuming that depletion is absent in galaxies with 12+logO/H = 7.0.”
The Primordial Abundance of 4He: A Self-consistent Empirical Analysis of Systematic Effects in a Large Sample of Low-Metallicity H II Regions (2007, background): “This is because the N/O abundance ratio tends to increase with increasing oxygen abundance (e.g., Izotov&Thuan 1999; Izotov et al. 2006).”
New fully empirical calibrations of strong-line metallicity indicators in star forming galaxies (2016, result): “The linear form of this relation, called t2-t3 relation , have been proposed for the first time by Campbell et al. (1986) and then revised in several studies (Garnett 1992; Izotov et al. 2006; Pilyugin et al. 2006b; Pilyugin 2006; Pilyugin et al. 2009, 2010a).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, methodology): “…star-forming galaxies provides a unique way to test the reliability of standard recipes based on the direct-Te method to measure element abundances from emission-line luminosities (e.g., Aller 1984; Garnett et al. 1995; Izotov & Thuan 1999; Izotov et al. 2006; Shapley et al. 2003; Erb et al. 2010).”