The spectrum of singly ionized gold, Au II

Rosberg, Maria; Wyart, J.-F.

doi:10.1088/0031-8949/55/6/009

Cited by 53 publications

(65 citation statements)

References 15 publications

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“…For Z 60, the np periapses were inside the 1s apiapses, whereas for Z 60 the np periapses were outside the 1s apiapses. Moreover, the transition Rosberg and Wyart (1997).…”

Section: Discussionmentioning

confidence: 99%

Experimental and theoretical studies of lifetimes and transition probabilities for AuII

Zhang¹,

Brage

Curtis

et al. 2002

J. Phys. B: At. Mol. Opt. Phys.

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We report lifetime measurements for three of the 5d 9 6p levels in Au II and relativistic multiconfiguration Dirac-Fock (MCDF) calculations of lifetimes and transitions probabilities in this ion. The work was motivated by significant disagreements between previous experimental 5d 9 6p lifetimes, obtained by means of the beam-foil (BF) method and theoretical data based on Hartree-Fock calculations in which relativistic effects were included as perturbations. The new measurements, based on laser-induced fluorescence, support the BF data and are also in excellent agreement with the MCDF results. We confirm that, while computational methods which include perturbative relativistic corrections appear to be adequate for moderately heavy elements such as Ag, fully relativistic calculations are essential for describing systems as heavy as Au.

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“…For Z 60, the np periapses were inside the 1s apiapses, whereas for Z 60 the np periapses were outside the 1s apiapses. Moreover, the transition Rosberg and Wyart (1997).…”

Section: Discussionmentioning

confidence: 99%

Experimental and theoretical studies of lifetimes and transition probabilities for AuII

Zhang¹,

Brage

Curtis

et al. 2002

J. Phys. B: At. Mol. Opt. Phys.

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“…The wording "not obs" is given for lines not present in the spectra, while the wordings "profile" and "blend" are given for lines observed well in the spectra but that do not have measurable equivalent widths either because the noise affects the profile too much or because other components affect the line. These wordings also indicate lines for which adequate equivalent widths cannot be computed as in the cases of Mg ii at 4481 Å, which is a blend of transitions belonging to the same multiplet, of most Mn ii lines which are affected by hyperfine structure, of the Ca ii infrared triplet which is a blend of isotopic Dworetsky et al (1984); (FW06 Ryabchikova & Smirnov (1994); (RW) Rosberg & Wyart (1997); (SL) Sigut & Landstreet (1990); K03Mn: http://kurucz.harvard.edu/atoms/2501/gf2501.pos; K03Ni: http://kurucz.harvard.edu/atoms/2801/gf2801. pos; K06: http://kurucz.harvard.edu/atoms/2701/gf2701.pos; K07F: http://kurucz.harvard.edu/atoms/2601/gf2601.pos.…”

Section: Discussionmentioning

confidence: 99%

A high-resolution study of isotopic composition and chemical abundances of blue horizontal branch stars in the globular clusters NGC 6397 and NGC 6752

Hubrig

Castelli

Silva

et al. 2009

A&A

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Aims. Large abundance anomalies have been previously detected in Horizontal Branch B-type stars. It has been suggested that at T eff > 11 000 K the stellar atmospheres become susceptible to diffusion effects and thus develop surface abundances similar to those that appear in the main-sequence, chemically peculiar group of A and B-type stars. We present the first high-resolution study of isotopic anomalies and chemical abundances in six Horizontal Branch B-type stars in globular clusters NGC 6397 and NGC 6752 and compare them to those observed in HgMn stars. Methods. We obtained high-resolution (up to R ∼ 115 000) UVES spectra of a representative sample of six B-type stars (T183, T191, T193, B652, B2151, B2206) with sharp spectral lines (v sin i ≤ 10 km s −1 ). The stars T183 and B2151 were observed on two consecutive nights to examine potential spectrum variability. A detailed spectrum analysis was done relying on Kurucz ATLAS9 and ATLAS12 models. The spectra were analysed using the SYNTHE code to generate synthetic spectra. Results. It is the first time an abundance analysis is performed for all elements for which spectral lines were detected in UVES spectra of Horizontal Branch B-type stars. Our study of these stars revealed no signs of He isotopic anomalies, which would produce a 3 He/ 4 He ratio different from the solar one. The isotopic anomaly of Ca is detected in all six studied stars. The chemical abundance analysis reveals an overabundance over the solar values of P, Ti, Mn, Fe, and Y and an overabundance over the cluster metallicity of Mg, Ca, and Cr. This behaviour is very similar in all six stars of both clusters with a few exceptions: the Na abundance is larger by more than 1.4 dex than the cluster metallicity in B652, and by more than 0.8 dex greater than the cluster metallicity in B2206; the Co abundance is 1.0 dex over the solar abundance for T191, while Zr is overabundant over the solar abundance by 0.4 dex in B2206. No lines of Hg or other heavy elements were observed in the spectra. Weak emission lines of Ti ii, similar to those frequently observed in HgMn stars have been discovered in one Horizontal Branch B-type star T191. Furthermore, we detected a radial velocity change of 0.9 km s −1 from one night to the next for T183 and 0.4 km s −1 for B2151. Further high-resolution observations are needed to examine whether both stars are spectroscopic binaries.

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“…The oscillator strength for the Au ii 1740Å line was obtained by combining theoretical branching ratios with measured lifetimes . Rosberg & Wyart (1997) performed an extensive study of the Au ii spectrum in the 800Å to 8000Å spectral region. They identified more than 500 spectral lines and calculated oscillator strengths for 497 lines using the Cowan codes.…”

Section: Elements Heavier Than Lu (Z > 71)mentioning

confidence: 99%

VALD–2: Progress of the Vienna Atomic Line Data Base

Kupka¹,

Piskunov²,

Ryabchikova³

et al. 1999

Astron. Astrophys. Suppl. Ser.

1,500

1,435

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Abstract. We describe the updated version of the "Vienna Atomic Line Data Base" (VALD, Piskunov et al. 1995) which represents a considerable improvement over the first installation from 1994. The original line lists have been complemented with critically evaluated data obtained from experimental measurements and theoretical calculations which are necessary for computing state-ofthe-art line opacities in stellar atmospheres, as well as for synthesizing spectra for high precision analyses. In this paper, we present new and improved data sets for neutral species and ions of Si, P, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Ru, Xe, La, Ce, Pr, Nd, Sm, Eu, Gd, Dy, Ho, Er, Tm, Yb, Lu, Re, Pt, Au, Hg, and Pb. For some species data are available in VALD for the first time. We explain our choice of quality rankings by reviewing the literature for the new data and by comparison with source lists included into VALD. For some cases, we produced new line data by weighted averaging of data from different sources with individual error estimates in order to increase the reliability of VALD line lists.Software modifications allow remote users of VALD to specify individual extraction parameters as an alternative to the default settings of the VALD team and to have direct control over the quality ranking of line data. A World-Wide-Web interface is described which provides easy access to all new features.To simplify proper crediting of all authors of atomic data, VALD now includes a compilation of all publications used in each type of reply.Finally, we briefly discuss the future roadmap of VALD developments, including the incorporation of molecular transitions and integration with external data bases.Send offprint requests to: F. Kupka

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The spectrum of singly ionized gold, Au II

Cited by 53 publications

References 15 publications

Experimental and theoretical studies of lifetimes and transition probabilities for AuII

Experimental and theoretical studies of lifetimes and transition probabilities for AuII

A high-resolution study of isotopic composition and chemical abundances of blue horizontal branch stars in the globular clusters NGC 6397 and NGC 6752

VALD–2: Progress of the Vienna Atomic Line Data Base

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