Theoretical values for the [O iii] 5007/4959 line-intensity ratio and homologous cases

By P. Storey, C. Zeippen. 2000

451 citations recorded by the source corpus.

Subfields: Atomic and Molecular Physics, and Optics, Mechanics of Materials

View Paper: https://www.semanticscholar.org/paper/60e8f9f78eba0b32033a3383d8dcd0608b5aab9d

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In Atomic and Molecular Physics, and Optics

1. G. D. Zanna
2. K. Dere
3. Peter R. Young
4. E. Landi
5. Helen E. Mason
6. T. Naab
7. Joss Bland-Hawthorn
8. R. Genzel

In Mechanics of Materials

1. G. D. Zanna
2. K. Dere
3. Peter R. Young
4. E. Landi
5. Helen E. Mason
6. M. Landini
7. Astronomy
8. Á. López-Sánchez

Citations in the corpus

• An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, methodology): “In parenthesis, the [O iii]λ4959 flux adopting the theoretical ratio [O iii]λ5007/[O iii]λ4959 = 3 (Storey & Zeippen 2000). b The emission line dust correction method is described in Appendix A. c FWHM (instrumental corrected) and error in units of km s−1. d Equivalent width and error in units of…”
• EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, background): “…of the narrow Hα, [N ii] and [S ii] line components are the same, and likewise for the broad components; 2. the ratio of [N ii] λ6548/λ6583 is 0.32 (Storey & Zeippen 2000); and 3. the flux ratio [S ii] λ6716/λ6731 in the broad component (if detected) is ∼1, similar to that found in the narrow…”
• GASP. I. Gas Stripping Phenomena in Galaxies with MUSE (2017, background): “Moreover, the flux ratios of the two [N II] and [O III] lines are kept constant in the fit assuming the ratios given in Storey & Zeippen (2000).”
• CHIANTI—An Atomic Database for Emission Lines. VI. Proton Rates and Other Improvements (2002, methodology): “G ri n & Badnell(2000) did not provide the forbidden radiative decay rates for the ground con guration and so we have adopted the data provided by Bhatia & Doschek (1993),exceptfor the 3P1;2{1D 2 transitionswhich com e from Storey & Zeippen (2000).”
• A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties (2023, background): “98 that is taken from theoretical calculations (Storey & Zeippen 2000).”
• GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, unknown): “In cases where [O iii]λ5007 is not well constrained by the data, but [O iii]λ4959 is, or vice versa, we assume that f[O iii(λ4959)] = 1/3 · f[O iii(λ5007)] (Storey & Zeippen 2000).”
• JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators (2023, unknown): “…estimating metallicities empirically, we require that the objects have coverage of the [ O III ] + H β emission lines in their spectra, and that the [ O III ] λλ 5007 / 4959 doublet line ratio is consistent with the theoretical value ( 2.98; Storey & Zeippen 2000 ) at a 2.5 σ signi fi cance level.”
• Galaxy And Mass Assembly (GAMA): Spectroscopic analysis (2013, background): “6 we show the distribution of [OIII]λ4956/[OIII] λ5007 compared to the expected ratio of1/2.98 (Storey & Zeippen 2000).”
• Line formation in solar granulation IV. (O I), O I and OH lines and the photospheric O abundance (2003, background): “185 (Storey & Zeippen 2000).”
• BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics (2017, background): “The intensity of [O III] λ4959 relative to [O III] λ5007 is fixed at the theoretical value of 2.98 (Storey & Zeippen 2000) and the intensity of [N II] λ6548 relative to [N II]λ6583 is set to the theoretical value of 2.96 (Acker et al. 1989).”
• CHIANTI - an atomic database for emission lines. IX. Ionization rates, recombination rates, ionization equilibria for the elements hydrogen through zinc and updated atomic data (2009, methodology): “The A-values for the ground configuration have been updated with the values of Tachiev & Froese Fischer (2001), except for the 2–4 and 3–4 transitions for which the previous data of Storey & Zeippen (2000) are retained.”
• The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, methodology): “The models were generated for the size, Sersic index, inclination, and dynamical mass derived from the data, with the line emission normalized to the source-integrated Hα flux, [N II]/Hα ratio, and assuming [N II]λ 6548/[N II]λ 6584 = 0.34 (Storey & Zeippen 2000).”
• THE FMOS-COSMOS SURVEY OF STAR-FORMING GALAXIES AT z ∼ 1.6. I. Hα-BASED STAR FORMATION RATES AND DUST EXTINCTION (2013, methodology): “We fix the width of all lines to be equivalent and the flux ratios [N II ]λ6583/[N II ]λ6548 and [OIII ]λ5007/[OIII ]λ4959 to the theoretical values of 2.96 and 2.98 (Storey & Zeippen 2000), respectively.”