E1 transitions of astrophysical interest in neutral oxygen

Hibbert, A; Biémont, Émile; Godefroid, Michel; Vaeck, Nathalie

doi:10.1088/0953-4075/24/18/010

Cited by 89 publications

(101 citation statements)

References 49 publications

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“…The latter is the same source used by the NIST database, and the later investigation of Tayal (2009) just confirms the reliability and high accuracy of their data. Transition data from Tayal (2009) agree with oscillator strengths f of Hibbert et al (1991) within 10%. We also tabulate oscillator strengths for two 2s -2p transition lines in Lilike O VI determined by Peach et al (1988).…”

Section: Oxygen Speciesmentioning

confidence: 75%

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Atomic Data Revisions for Transitions Relevant to Observations of Interstellar, Circumgalactic, and Intergalactic Matter

Cashman

Kulkarni

Kisielius

et al. 2017

ApJS

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Measurements of element abundances in galaxies from astrophysical spectroscopy depend sensitively on the atomic data used. With the goal of making the latest atomic data accessible to the community, we present a compilation of selected atomic data for resonant absorption lines at wavelengths longward of 911.753Å (the H I Lyman limit), for key heavy elements (heavier than atomic number 5) of astrophysical interest. In particular, we focus on the transitions of those ions that have been observed in the Milky Way interstellar medium (ISM), the circumgalactic medium (CGM) of the Milky Way and/or other galaxies, and the intergalactic medium (IGM). We provide wavelengths, oscillator strengths, associated accuracy grades, and references to the oscillator strength determinations. We also attempt to compare and assess the recent oscillator strength determinations. For about 22% of the lines that have updated oscillator strength values, the differences between the former values and the updated ones are 0.1 dex. Our compilation will be a useful resource for absorption line studies of the ISM, as well as studies of the CGM and IGM traced by sight lines to quasars and gamma-ray bursts. Studies (including those enabled by future generations of extremely large telescopes) of absorption by galaxies against the light of background galaxies will also benefit from our compilation.

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Section: Oxygen Speciesmentioning

confidence: 75%

“…For other lines not covered by Froese Fischer & Tachiev (2004), we use data from Butler & Zeippen (1991) and Hibbert et al (1991). The latter is the same source used by the NIST database, and the later investigation of Tayal (2009) just confirms the reliability and high accuracy of their data.…”

Section: Oxygen Speciesmentioning

confidence: 99%

Atomic Data Revisions for Transitions Relevant to Observations of Interstellar, Circumgalactic, and Intergalactic Matter

Cashman

Kulkarni

Kisielius

et al. 2017

ApJS

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“…We tested the convergence of close-coupling expansion for collision strengths of low-lying transitions by performing progressively larger 3-state, 16-state, and 26-state calculations. We included 21 spectroscopic 2s 2 2p 4 3 P, Nahar (1998) and Hibbert et al (1991) and the experimental values of Brooks, Rohrlich, & Smith (1977), Smith et al (1971), Bromander et al (1978), Day, Anderson, & Salamo (1981), and Kroll et al (1985). Our results are in excellent agreement with the theoretical values of Nahar (1998) and Hibbert et al (1991) 4 configuration and from these states to the excited states of the 2s 2 2p 3 ns (n ¼ 3 5), 2s 2 2p 3 np (n ¼ 3 4), 2s 2 2p 3 nd (n ¼ 3 4), 2s 2 2p 3 4f , and 2s2p 5 configurations.…”

Section: Discussion Of the Resultsmentioning

confidence: 99%

Electron Collisional Excitation Rates for O i Using the B ‐Spline R ‐Matrix Approach

Zatsarinny

Tayal

2003

ASTROPHYS J SUPPL S

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The B-spline R-matrix approach has been used to calculate electron collisional excitation strengths and rates for transitions between the 3 P, 1 D, and 1 S states of ground configuration and from these states to the states of the excited 2s 2 2p 3 ns (n ¼ 3 5), 2s 2 2p 3 np (n ¼ 3 4), 2s 2 2p 3 nd (n ¼ 3 4), 2s 2 2p 3 4f , and 2s2p 5 configurations. The nonorthogonal orbitals are used for an accurate description of both the target wave functions and the R-matrix basis functions. The thermally averaged collision strengths are obtained from the collision strengths by integrating over a Maxwellian velocity distribution of electron energies, and these are tabulated over a temperature range from 1000 to 60,000 K. The parametric functions of scaled energy have also been obtained to represent collision strengths over a wide energy range or thermally averaged collision strengths at any desired temperature.

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“…Line data used in the analysis are given in Table 2. The g f values of the C i lines are based on quantum mechanical calculations by Hibbert et al (1993) and those of oxygen are taken from Hibbert et al (1991). Doppler broadening by non-thermal, small-scale motions in the atmosphere is described by one parameter, ξ turb , in the usual way.…”

Section: Model Atmospheres and Line Broadeningmentioning

confidence: 99%

The carbon-to-oxygen ratio in stars with planets

Nissen

2013

A&A

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Context. In some recent works, the C/O abundance ratio in high-metallicity stars with planets is found to vary by more than a factor of two, i.e. from ∼0.4 to C/O 1. This has led to discussions about the existence of terrestrial planets with a carbon-dominated composition that is very different from the composition of the Earth.Aims. The mentioned C/O values were obtained by determining carbon abundances from high-excitation C i lines and oxygen abundances from the forbidden [O i] line at 6300 Å. This weak line is, however, strongly affected by a nickel blend at high metallicities.Aiming for more precise C/O ratios, oxygen abundances in this paper are derived from the high-excitation O i triplet at 7774 Å. Methods. The C i lines at 5052 and 5380 Å in HARPS spectra were applied to determine carbon abundances of 33 solar-type stars for which FEROS spectra are available for determining oxygen abundances from the O i λ7774 triplet. Differential abundances with respect to the Sun were derived from equivalent widths using MARCS model atmospheres. Non-LTE corrections were included, and the analysis was carried out with both spectroscopic and photometric estimates of stellar effective temperatures and surface gravities.

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E1 transitions of astrophysical interest in neutral oxygen

Cited by 89 publications

References 49 publications

Atomic Data Revisions for Transitions Relevant to Observations of Interstellar, Circumgalactic, and Intergalactic Matter

Atomic Data Revisions for Transitions Relevant to Observations of Interstellar, Circumgalactic, and Intergalactic Matter

Electron Collisional Excitation Rates for O i Using the B ‐Spline R ‐Matrix Approach

The carbon-to-oxygen ratio in stars with planets

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