Atlas of the spectrum of a platinum neon hollow-cathode reference lamp in the region 1130-4330 angstrom

Sansonetti, Jean E.; Reader, Joseph; Sansonetti, Craig J.; Acquista, Nicolo

doi:10.6028/jres.097.002

Cited by 65 publications

(65 citation statements)

References 18 publications

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“…In the same paper, Wahlgren et al report on calculated oscillator strength for the Pt ii line at 2144.25Å which turned out to be slightly larger than the relative astrophysical log gf -value derived by Dworetsky et al (1984). Soon after, Wyart & Blaise (1995) published an extensive study of the Pt ii spectrum based on the atlas of Sansonetti et al (1992). Wyart & Blaise calculated the transition probabilities for 112 lines in the 1380Å to 2800Å spectral region and also provided theoretical Landé factors for the odd energy levels.…”

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

confidence: 95%

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

Kupka¹,

Piskunov²,

Ryabchikova³

et al. 1999

Astron. Astrophys. Suppl. Ser.

1,509

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

confidence: 95%

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

Kupka¹,

Piskunov²,

Ryabchikova³

et al. 1999

Astron. Astrophys. Suppl. Ser.

1,509

1,435

View full text Add to dashboard Cite

show abstract

“…Observed intensities of platinum lines from this lamp were compared to the calibrated intensities in the atlas of the Pt-Ne lamp (Sansonetti et al 1992) to estimate the instrumental response function of the FTS for each of the two output ports and detectors. These instrumental response functions were applied to the initial intensities for the Cr-Ne lamp to obtain roughly calibrated values.…”

Section: Methodsmentioning

confidence: 99%

“…Line intensities were recorded as visual estimates of the photographic plate blackening. The spectra were calibrated using reference spectra of Pt i and Pt ii (Sansonetti et al 1992). For sharp well-exposed lines, the typical uncertainty of the measurements is 0.002 Å.…”

Section: Methodsmentioning

confidence: 99%

COMPREHENSIVE OBSERVATIONS OF THE ULTRAVIOLET SPECTRUM AND IMPROVED ENERGY LEVELS FOR SINGLY IONIZED CHROMIUM (Cr II)

Sansonetti

Nave

Reader

et al. 2012

ApJS

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We report new observations of the spectrum of singly ionized chromium (Cr ii) in the region 1142-3954 Å. The spectra were recorded with the National Institute of Standards and Technology 10.7 m normal-incidence vacuum spectrograph and FT700 vacuum ultraviolet Fourier transform spectrometer. More than 3600 lines are classified as transitions among 283 even and 368 odd levels. The new spectral data are used to re-optimize the energy levels, reducing their uncertainties by a typical factor of 20.

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“…The Kurucz compilation of atomic line data in this region was supplemented by data for several elements important to both the immediate problem of line blending with the Au ii line(s) and defining the continuum level. These spectral studies included Fe ii ( Nave et al 1997), Fe iii ( Ekberg 1993), Cr iii ( Ekberg 1997), Y ii ( Nilsson et al 1991), Ni ii ( Fedcheck & Lawler 1999), and Pt i /ii /iii (Sansonetti et al 2003, originally published as Sansonetti et al 1992). In addition, the known spectra of other first ions were checked for lines in this area, but none were found to contribute to observable features.…”

Section: Example: the Treatment Of Au IImentioning

confidence: 99%

Heavy Element Abundances in Late‐B and Early‐A Stars. I. Co‐AddedIUESpectra of HgMn Stars

Adelman¹,

Proffitt²,

Wahlgren³

et al. 2004

ASTROPHYS J SUPPL S

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Very heavy elements ( Pt, Au, Hg, Tl, and Bi) are found to be enhanced in the atmospheres of the chemically peculiar stars of the upper main sequence by up to a million times the solar system levels. Such enhancements are believed to result from atmospheric dynamics (i.e., diffusion) rather than scenarios that dredge up nuclearprocessed material to the surface or transfer processed material between binary companions. However, the theoretical framework needs to be further constrained by observations beyond the realm of the spectral types for which such abundance enhancements are observed at optical wavelengths.The International Ultraviolet Explorer (IUE ) satellite collected spectra of bright stars for which chemical peculiarities have been derived from ground-based data. For several elements the abundance enhancements have only been recently measured using Hubble Space Telescope data and have therefore not yet been exploited in the IUE data. We have initiated a program to analyze IUE high-dispersion spectra to more fully characterize the pattern of very heavy element enhancement for many mercury-manganese ( HgMn) stars and to potentially extend the spectral class (effective temperature) boundaries over which these abundance anomalies are known to exist. The abundances of very heavy elements in chemically normal B and A-type stars provide a base level that may be compared with the solar system abundances. These early spectral type stars may therefore reveal clues for galactic chemical evolution studies since they were formed at a later epoch than the Sun in the history of the Galaxy. This first paper presents the motivation for the analyses to follow, outlines our spectral co-addition technique for IUE spectra, and discusses the choice of model atmospheres and the synthetic spectrum procedures, while initiating the study by highlighting the abundance of gold in several HgMn stars.

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Atlas of the spectrum of a platinum neon hollow-cathode reference lamp in the region 1130-4330 angstrom

Cited by 65 publications

References 18 publications

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

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

COMPREHENSIVE OBSERVATIONS OF THE ULTRAVIOLET SPECTRUM AND IMPROVED ENERGY LEVELS FOR SINGLY IONIZED CHROMIUM (Cr II)

Heavy Element Abundances in Late‐B and Early‐A Stars. I. Co‐AddedIUESpectra of HgMn Stars

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