Hyperfine structures and isotopic shifts of the Cu D1 and D2 lines measured by high-resolution laser fluorescence spectroscopy with a collimated atomic beam

Hermann, G.; Lasnitschka, G.; Schwabe, C.; Spengler, D.

doi:10.1016/0584-8547(93)80110-g

Cited by 19 publications

(13 citation statements)

References 13 publications

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“…A B Level 1.710 0.0059 -0.008 a P 1.740 0.0106 0.004 a P 1.785 -0.0236 0.0 a P 1.883 0.0374 0.005 b 4 P 1.956 0.0154 -0.002 b 4 P 2.042 0.0205 0.002 a G 2.080 0.0463 0.004 a D 2.137 0.028 -0.0032 a G 2.280 0.0112 0.004 a P 2.328 0.0201 0.0 a P 3.117 0.0253 0.008 z G 3.216 0.0206 0.005 z G 3.252 0.0183 0.006 z G 3.298 0.0049 0.004 z G 3.514 0.0270 -0.002 z F 3.576 0.0258 0.007 z G 3.629 0.0173 0.006 z G 3.632 0.0251 0.00 z 0.042 0.00 y D 5.552 0.0134 0.00 e F 5.663 0.0335 0.005 e F 5.791 0.0287 -0.001 e F 5.839 0.0257 -0.001 e F 5.873 0.0194 -0.001 e F 5.892 0.0360 0.005 f F 5.976 0.0283 0.003 f F 6.341 0.0000 0.0 e H 6.345 0.0000 0.00 e H 6.348 0.0000 0.00 e G 6.462 0.0000 0.00 e H 6.543 0.0000 0.00 e G Article number, page 66 of 76 Heiter et al: Atomic data for the Gaia-ESO Survey Kurucz (2012), Wagner (1955 3.786 0.0169 0.0 -0.0059 0.0181 0.0 0.0132 4p 2 P Hermann et al (1993) Kurucz (2012, Wagner (1955) 3.817 0.0065 -0.0010 -0.0062 0.0069 -0.0009 0.0139 4p 2 P Hermann et al (1993) Kurucz (2012), Wagner (1955 0.0 0.0 -0.006 0.0 0.0 0.013 4d 2 D none Kurucz (2012) Notes. (a) http://kurucz.harvard.edu/atoms/2900/ab290063.dat, http://kurucz.harvard.edu/atoms/2900/ab290065.dat D Höhle et al (1982) 0.235 −3.760 × 10 −2 1.66 × 10 −3 6s a 3 D Höhle et al (1982) 0.244 −6.19 × 10 −4 1.25 × 10 −3 5d 2 a 3 F Höhle et al (1982) 0.321 −3 × 10 −4 1.89 × 10 −3 6s a 3 D Höhle et al (1982) 2.261 4.96 × 10 −3 1.5 × 10 −4 5d y 3 F o Höhle et al (1982) 2.658 1.44 × 10 K Rivest et al (2002) 3.170 2.301 × 10 −2 6p 5 K Rivest et al (2002) 3.363 1.973 × 10 −2 6p 5 K Rivest et al (2002) Article number, page 67 of 76…”

Section: E (Ev)mentioning

confidence: 99%

Atomic data for the Gaia-ESO Survey

Heiter

Lind

Bergemann

et al. 2021

A&A

136

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: E (Ev)mentioning

confidence: 99%

Atomic data for the Gaia-ESO Survey

Heiter

Lind

Bergemann

et al. 2021

A&A

136

142

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show abstract

“…12 The resulting lines are separated by more than a Doppler width, but are resolved only in very high resolution experiments. 13 In addition, the isotope effect for copper ͓ 29 Cu 63 ͑69.09%͒ and 29 Cu 65 ͑30.91%͔͒ doubles the number of lines. Because the hyperfine lines are separated in frequency by more than a Doppler width, the multiplet structure must be explicitly treated in our curve of growth method in order to obtain accurate ground state copper atom densities, even though the hyperfine structure is not resolved at our instrumental resolution.…”

Section: A Hyperfine Structure Of Ground State Copper Absorption Linementioning

confidence: 99%

Absolute densities of long lived species in an ionized physical vapor deposition copper–argon plasma

Andrew

Abraham

Booske

et al. 2000

Journal of Applied Physics

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Optical absorption spectroscopy has been used to measure absolute, average gas phase densities of neutral copper, ground and metastable states, and neutral argon, metastable and resonance states, in an ionized physical vapor deposition plasma. Spectroscopic measurements were carried with a xenon arc lamp as a high intensity, continuum light source, and an optical multichannel detector. Copper radiative transitions in the wavelength range of 324.8-510.6 nm and argon radiative transitions in the 706.7-811.5 nm range were employed. The curve of growth method has been used to calculate the absolute line average densities from fractional absorption data. For a copper-argon plasma of neutral pressure 30 and 10 mTorr copper metastable state densities were found to lie in the range of 10 10 -10 12 cm Ϫ3 . Comparison of these densities with neutral copper densities derived from independent measurements of neutral copper flux at the substrate indicate gas phase temperatures greater than 1500 K under certain experimental conditions. These values of inferred temperatures indicate the copper metastable state density to be significant in comparison with neutral copper ground state densities at 10 and 30 mTorr with radio frequency heating power of 1 kW. The concentrations of argon 4s sublevels of the first excited state were found to be in the range of 4.5ϫ10 8 -1.5ϫ10 11 cm Ϫ3 for the experimental conditions studied. The ordering of the relative densities of the argon 4s sublevels and the variation of the lumped first excited state with experimental parameters are discussed.

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“…There are two isotopes of copper, 57 Cu and 59 Cu, both affected by HFS. The HFS and IS information was taken from Hermann et al (1993), and the ratio of the isotopes seen in the solar system was used. Unfortunately, the S/N in this region is $25, even after co-adding the spectra from overlapping orders.…”

Section: Appendix a Atomic Parameters Oscillator Strengths And Line mentioning

confidence: 99%

Thes‐Process in Metal‐Poor Stars: Abundances for 22 Neutron‐Capture Elements in CS 31062‐050

Johnson

Bolte

2004

ApJ

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The CH star CS 31062-050 (½Fe=H ¼ À2:42) is one of the most useful stars yet discovered for evaluating the s-process in metal-poor stars. It is very abundant in heavy elements (e.g., ½La=Fe ¼ 2:2), and its relatively cool temperature and low gravity mean that there are many lines of interesting elements present in the spectrum. We measured the abundances of 22 elements with Z ! 29, including the rarely measured Lu and Pd. We derive an upper limit on the Th abundance as well. The abundances in CS 31062-050 show a similar pattern to many other metal-poor CH stars: high [Pb/Fe] and [Pb/La] ratios, low [Y/La] ratios and high [Eu/La] values compared to the solar system s-process. However, the Th limit, with additional assumptions, is not consistent with the idea that the excess Eu in CS 31062-050 is contributed by the r-process. In addition, the observed [Eu/Tb] cannot be explained by any ratio of solar-system s-process and r-process abundances. We therefore argue that the abundance pattern in CS 31062-050 is most likely the result of the s-process, and we discuss possible modifications that could explain the non-solar-system pattern observed.

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Hyperfine structures and isotopic shifts of the Cu D1 and D2 lines measured by high-resolution laser fluorescence spectroscopy with a collimated atomic beam

Cited by 19 publications

References 13 publications

Atomic data for the Gaia-ESO Survey

Atomic data for the Gaia-ESO Survey

Absolute densities of long lived species in an ionized physical vapor deposition copper–argon plasma

Thes‐Process in Metal‐Poor Stars: Abundances for 22 Neutron‐Capture Elements in CS 31062‐050

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