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

Storey, P. J.; Zeippen, C. J.

doi:10.1046/j.1365-8711.2000.03184.x

Cited by 527 publications

(427 citation statements)

References 11 publications

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“…The I(630.0 nm)/I(636.4 nm) is equal to 2.997 ± 0.016 and can be compared to the ratio of 2.997 determined by Storey and Zeippen [2000] in a recent set of calculations. The same calculation procedure gives a value of 14.2 for the O( 1 S) case [Galavis et al, 1997], this value being somewhat lower than most theoretical determinations (Table 1).…”

Section: Introductionmentioning

confidence: 90%

O(¹S → ¹D,³P) branching ratio as measured in the terrestrial nightglow

et al. 2006

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[1] The branching ratio of the two optically forbidden atmospheric emission lines, O( 1 S À 1 D) at 557.7 nm and O( 1 S À 3 P) at 297.2 nm, is a fixed number in the upper atmosphere because the O( 1 S) level is common to both lines. The value for the ratio A(557.7)/A(297.2) currently recommended by NIST is 16.7, and the ratio found in the laboratory is somewhat larger. Field observations require space-based instruments, in which case calibration between the two wavelength regions is the critical issue. We circumvent this problem by using the O 2 (A-X) Herzberg I emission system as a bridge between the UV region below 310 nm and the ground-accessible region above that wavelength. These two spectral regions can be separately calibrated in terms of intensity, and the results of a disparate set of observations (satellite, rocket, ground-based sky spectra) lead to a quite consistent value of 9.8 ± 1.0 for A(557.7)/A(297.2). This conclusion has consequences for auroral and dayglow processes and for spectral calibration. It is particularly important to ascertain the cause of the substantial difference between this value and those from theory.

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Section: Introductionmentioning

confidence: 90%

O(¹S → ¹D,³P) branching ratio as measured in the terrestrial nightglow

et al. 2006

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“…(iv) [O III] is a doublet; each member is fitted with a single Gaussian, tied together in velocity width, and with an amplitude ratio of 2.98 (Storey & Zeippen 2000).…”

Section: Optical/ir Spectral Fittingmentioning

confidence: 99%

Reaching the peak of the quasar spectral energy distribution – I. Observations and models

Collinson

Ward

Done

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We perform a spectral analysis of a sample of 11 medium redshift (1.5 z 2.2) quasars. Our sample all have optical spectra from the SDSS, infrared spectra from GNIRS and TSPEC, and X-ray spectra from XMM-Newton. We first analyse the Balmer broad emission line profiles which are shifted into the IR spectra to constrain black hole masses. Then we fit an energy-conserving, three component accretion model of the broadband spectral energy distribution (SED) to our multiwavelength data. Five out of the 11 quasars show evidence of an SED peak, allowing us to constrain their bolometric luminosity from these models and estimate their mass accretion rates. Based on our limited sample, we suggest that estimating bolometric luminosities from L 5100 Å and L 2−10 keV may be unreliable, as has been also noted for a low-redshift, X-ray selected AGN sample.

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“…The adopted f -values are from Storey & Zeippen (2000). The damping parameters have no influence on the profile of these weak lines.…”

Section: Atomic Data and Model Atmospheresmentioning

confidence: 99%

The photospheric solar oxygen project

Caffau

Ludwig

Steffen

et al. 2015

A&A

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Context. The solar photospheric abundance of oxygen is still a matter of debate. For about ten years some determinations have favoured a low oxygen abundance which is at variance with the value inferred by helioseismology. Among the oxygen abundance indicators, the forbidden line at 630 nm has often been considered the most reliable even though it is blended with a Ni i line. In Papers I and II of this series we reported a discrepancy in the oxygen abundance derived from the 630 nm and the subordinate [O I] line at 636 nm in dwarf stars, including the Sun. Aims. Here we analyse several, in part new, solar observations of the centre-to-limb variation of the spectral region including the blend at 630 nm in order to separate the individual contributions of oxygen and nickel. Methods. We analyse intensity spectra observed at different limb angles in comparison with line formation computations performed on a CO5BOLD 3D hydrodynamical simulation of the solar atmosphere. Results. The oxygen abundances obtained from the forbidden line at different limb angles are inconsistent if the commonly adopted nickel abundance of 6.25 is assumed in our local thermodynamic equilibrium computations. With a slightly lower nickel abundance, A(Ni) ≈ 6.1, we obtain consistent fits indicating an oxygen abundance of A(O) = 8.73 ± 0.05. At this value the discrepancy with the subordinate oxygen line remains. Conclusions. The derived value of the oxygen abundance supports the notion of a rather low oxygen abundance in the solar photosphere. However, it is disconcerting that the forbidden oxygen lines at 630 and 636 nm give noticeably different results, and that the nickel abundance derived here from the 630 nm blend is lower than expected from other nickel lines.

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

Cited by 527 publications

References 11 publications

O(¹S → ¹D,³P) branching ratio as measured in the terrestrial nightglow

O(¹S → ¹D,³P) branching ratio as measured in the terrestrial nightglow

Reaching the peak of the quasar spectral energy distribution – I. Observations and models

The photospheric solar oxygen project

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

Cited by 527 publications

References 11 publications

O(1S → 1D,3P) branching ratio as measured in the terrestrial nightglow

O(1S → 1D,3P) branching ratio as measured in the terrestrial nightglow

Reaching the peak of the quasar spectral energy distribution – I. Observations and models

The photospheric solar oxygen project

Contact Info

Product

Resources

About

O(¹S → ¹D,³P) branching ratio as measured in the terrestrial nightglow

O(¹S → ¹D,³P) branching ratio as measured in the terrestrial nightglow