Hyperfine structure of CW dye laser populated high lying levels of 45Sc by atomic-beam magnetic-resonance

Zeiske, W.; Meisel, G.; Gebauer, H.; Höfer, Bianca; Ertmer, W.

doi:10.1016/0375-9601(75)90562-9

Cited by 22 publications

(11 citation statements)

References 2 publications

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“…Article number, page 53 of 76 Hofer (1976) 1.851 0.0100 0.0000 4s 2 F Başar et al 20041.865 -0.0008 0.0000 4s 2 F Başar et al 20041.996 -0.0115 0.0000 4p 2 D Başar et al 20043.619 0.0029 0.0000 4p 4 G Başar et al 20043.633 0.0015 0.0000 4p 4 G Başar et al 20043.878 0.0019 0.0000 4p 4 F Öztürk et al (2007) 4.110 0.0034 0.0000 4p 2 G Öztürk et al (2007) 4.111 0.0071 0.0000 4p 2 F Öztürk et al (2007) 4.179 0.0015 0.0000 4p 2 D Başar et al 2004Article number, page 63 of 76…”

Section: Appendix A: Auxiliary Tablesmentioning

confidence: 99%

“…Childs (1971) employed the atomic-beam magnetic-resonance technique (ABMR) resulting in highly accurate data for the 3d4s 2 2 D 3/2,5/2 levels. ABMR data were also presented by Ertmer & Hofer (1976) and Zeiske et al (1976) for the ( 3 F)4s 4 F 3/2,5/2,7/2,9/2 levels, which we employ. For several others, including the ( 3 F)4s 2 F 5/2,7/2 levels, the only source of data are the calculations published by Başar et al (2004).…”

Section: Appendix B11: Scandium (Z=21)mentioning

confidence: 99%

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Atomic data for the Gaia-ESO Survey

Heiter

Lind

Bergemann

et al. 2021

A&A

129

142

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Context. We describe the atomic and molecular data that were used for the abundance analyses of FGK-type stars carried out within the Gaia-ESO Public Spectroscopic Survey in the years 2012 to 2019. The Gaia-ESO Survey is one among several current and future stellar spectroscopic surveys producing abundances for Milky-Way stars on an industrial scale. Aims. We present an unprecedented effort to create a homogeneous common line list, which was used by several abundance analysis groups using different radiative transfer codes to calculate synthetic spectra and equivalent widths. The atomic data are accompanied by quality indicators and detailed references to the sources. The atomic and molecular data are made publicly available in electronic form. Methods. In general, experimental transition probabilities were preferred but theoretical values were also used. Astrophysical g fvalues were avoided due to the model-dependence of such a procedure. For elements whose lines are significantly affected by a hyperfine structure or isotopic splitting, a concerted effort has been made to collate the necessary data for the individual line components. Synthetic stellar spectra calculated for the Sun and Arcturus were used to assess the blending properties of the lines. We also performed a detailed investigation of available data for line broadening due to collisions with neutral hydrogen atoms. Results. Among a subset of over 1300 lines of 35 elements in the wavelength ranges from 475 nm to 685 nm and from 850 nm to 895 nm, we identified about 200 lines of 24 species which have accurate g f-values and are free of blends in the spectra of the Sun and Arcturus. For the broadening due to collisions with neutral hydrogen, we recommend data based on Anstee-Barklem-O'Mara theory, where possible. We recommend avoiding lines of neutral species for which these are not available. Theoretical broadening data by R.L. Kurucz should be used for Sc ii, Ti ii, and Y ii lines; additionally, for ionised rare-earth species, the Unsöld approximation with an enhancement factor of 1.5 for the line width can be used. Conclusions. The line list has proven to be a useful tool for abundance determinations based on the spectra obtained within the Gaia-ESO Survey, as well as other spectroscopic projects. Accuracies below 0.2 dex are regularly achieved, where part of the uncertainties are due to differences in the employed analysis methods. Desirable improvements in atomic data were identified for a number of species, most importantly Al i, S i, and Cr ii, but also Na i, Si i, Ca ii, and Ni i.

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Section: Appendix A: Auxiliary Tablesmentioning

confidence: 99%

Section: Appendix B11: Scandium (Z=21)mentioning

confidence: 99%

Atomic data for the Gaia-ESO Survey

Heiter

Lind

Bergemann

et al. 2021

A&A

129

142

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“…We have synthesized the spectra in the Na I region after including the hyperfine structure for the Sc I 22058 and 22071 Å lines. The hfs constants for these transitions were taken from Zeiske et al (1976), Aboussäid et al (1996). The relative strengths of the hyperfine components were calculated following Tolansky (1948), and the absolute gf-values were calibrated against Arcturus, adopting [Sc/H] = -0.19 (McWilliam & Rich 1994).…”

Section: Comparison To the Low-resolution Spectroscopymentioning

confidence: 99%

The First Stellar Abundance Measurements in the Galactic Center: The M Supergiant IRS 7

Carr

Sellgren

Balachandran

2000

ApJ

136

157

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The first measurement of the photospheric abundances in a star at the Galactic Center are presented. A detailed abundance analysis of the Galactic Center M2 supergiant IRS 7 was carried out using high-resolution near-infrared echelle spectra. The Fe abundance for IRS 7 was found to be close to solar, [Fe/H] = -0.02 ± 0.13, and nearly identical to the Fe abundances we obtained for the nearby M supergiants α Ori and VV Cep. Analysis of the first and second overtone lines of CO was used to derive an effective temperature of 3600 ± 230 K, a microturbulent velocity of 3.0 ± 0.3 km s -1 , and a carbon abundance log ε(C) = 7.78 ± 0.13, or [C/H] = -0.77. In addition, we find a high depletion of 0.74 ± 0.32 dex in O and an enhancement of 0.92 ± 0.18 dex in N. These abundances are consistent with the dredge-up of CNO-cycle products but require deep mixing in excess of that predicted by standard models for red supergiants. In light of our measured solar Fe abundance for IRS 7, we discuss other indicators of metallicity at the Galactic Center, the interpretation of low-resolution near-infrared spectra of late-type giants and supergiants, including the need for caution in using such spectra as measures of metallicity, and the evolution of massive young stars at the Galactic Center. We suggest the possibility that rapid stellar rotation is common for stars formed under conditions in the Galactic Center, and that extra internal mixing induced by high rotation rates, rather than evolution at high metallicity, is the explanation for many of the unusual properties of the hot emission-line stars in the Galactic Center.

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“…High precision hyperfine structure experimental data were obtained by Childs [11], Zeiske et al [12] and Ertmer and Hofer [13] with the use of the atomic beam magnetic resonance method. For the ground configuration 3d4s 2 , one off-diagonal magnetic dipole hyperfine structure constant was determined by Childs [11] and later by Gebauer et al [14], who managed to reduce the uncertainty by an order of magnitude.…”

Section: Introductionmentioning

confidence: 99%