Tables of spectral-line intensities :

Meggers, William F.; Corliss, Charles; Scribner, Bourdon F.

doi:10.6028/nbs.mono.145p2

Cited by 101 publications

(128 citation statements)

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“…VALD-3 is a compilation of the work of many researchers, with parameters for some lines coming from multiple sources. The largest contributors to information in our line list (∼ 85% of the parameters) were from Kurucz (2010bKurucz ( , 2007Kurucz ( , 2010c; Davis et al (1986); Kurucz (1995Kurucz ( , 2013Kurucz ( , 2009); Raassen & Uylings (1998); Kurucz (2010aKurucz ( , 2008; Palmeri et al (2000); ; Goldman et al (1998);Meggers et al (1975); Barklem & Aspelund-Johansson (2005).…”

Section: Spectral Line Parametersmentioning

confidence: 99%

Spectral Properties of Cool Stars: Extended Abundance Analysis of 1,617 Planet-Search Stars

Brewer¹,

Fischer²,

Valenti³

et al. 2016

ApJS

382

451

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We present a catalog of uniformly determined stellar properties and abundances for 1,617 F, G, and K stars using an automated spectral synthesis modeling procedure. All stars were observed using the HIRES spectrograph at Keck Observatory. Our procedure used a single line list to fit model spectra to observations of all stars to determine effective temperature, surface gravity, metallicity, projected rotational velocity, and the abundances of 15 elements (C, N, O, Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Fe, Ni, & Y). Sixty percent of the sample had Hipparcos parallaxes and V-band photometry which we combined with the spectroscopic results to obtain mass, radius, and luminosity. Additionally, we used the luminosity, effective temperature, metallicity and α-element enhancement to interpolate in the Yonsei-Yale isochrones to derive mass, radius, gravity, and age ranges for those stars. Finally, we determined new relations between effective temperature and macroturbulence for dwarfs and subgiants. Our analysis achieved precisions of 25 K in T eff , 0.01 dex in [M/H], 0.028 dex for log g and 0.5 km s −1 in v sin ibased on multiple observations of the same stars. The abundance results were similarly precise, between ∼ 0.01 and ∼ 0.04 dex, though trends with respect to T eff remained for which we derived empirical corrections. The trends, though small, were much larger than our uncertainties and are shared with published abundances. We show that changing our model atmosphere grid accounts for most of the trend in [M/H] between 5000 K and 5500 K indicating a possible problem with the atmosphere models or opacities.

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Section: Spectral Line Parametersmentioning

confidence: 99%

Spectral Properties of Cool Stars: Extended Abundance Analysis of 1,617 Planet-Search Stars

Brewer¹,

Fischer²,

Valenti³

et al. 2016

ApJS

382

451

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“…Uncertainties in the log(gf ) values for the elements of interest generally do not contribute significantly to the abundance uncertainties. The Ge i, As i, and Se i transitions used in this study are all major branches(Meggers et al 1975) Wiese & Martin (1980). estimate accuracies of 25% (≤ 0.10 dex) for the Ge i transition probabilities.…”

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confidence: 99%

Germanium, Arsenic, and Selenium Abundances in Metal-Poor Stars*

Roederer

2012

ApJ

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The elements germanium (Ge, Z = 32), arsenic (As, Z = 33), and selenium (Se, Z = 34) span the transition from charged-particle or explosive synthesis of the iron-group elements to neutroncapture synthesis of heavier elements. Among these three elements, only the chemical evolution of germanium has been studied previously. Here we use archive observations made with the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope and observations from several ground-based facilities to study the chemical enrichment histories of seven stars with metallicities −2.6 ≤ [Fe/H] ≤ −0.4. We perform a standard abundance analysis of germanium, arsenic, selenium, and several other elements produced by neutron-capture reactions. When combined with previous derivations of germanium abundances in metal-poor stars, our sample reveals an increase in the [Ge/Fe] ratios at higher metallicities. This could mark the onset of the weak s-process contribution to germanium. In contrast, the [As/Fe] and [Se/Fe] ratios remain roughly constant. These data do not directly indicate the origin of germanium, arsenic, and selenium at low metallicity, but they suggest that the weak and main components of the s-process are not likely sources.

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“…The best lines for the analysis of Chromium, Cobalt, Vanadium, Manganese and Aluminum have been selected [18] using ICP -AES at the operating conditions listed in Table (2). The spectrum for each of these lines has been recorded at high (0.08 Å) and low (2 Å) resolution by changing the slit widths of the spectrometer.…”

Section: Study Of Spectral Interferences and Line Selection For Steelmentioning

confidence: 99%

Study of Spectral Interferences and Line Selection for Steel Analysis Using Inductively Coupled Plasma Atomic Emission Spectrometry ICP-AES

Ziara¹

2017

DJPS

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This paper is devoted to spectral interference studies and line selection for Inductively Coupled Plasma Atomic Emission Spectrometry (ICP-AES) when a low resolution spectrometer (∆λ min = 2 Å) is used for steel analysis. It has been identified that some of the most intense lines for Cobalt, Zirconium, Lead, Nickel, Niobium and Molybdenum at low resolution cannot be used owing to spectral interferences. Different interference free lines for Cobalt, Chromium, Vanadium, Nickel, Molybdenum and Manganese have therefore been selected. The possibility of differentiating different types of steel by recording their spectrum at particular regions of wavelength corresponding to their elemental composition has also been demonstrated in this paper.

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Tables of spectral-line intensities :

Cited by 101 publications

References 0 publications

Spectral Properties of Cool Stars: Extended Abundance Analysis of 1,617 Planet-Search Stars

Spectral Properties of Cool Stars: Extended Abundance Analysis of 1,617 Planet-Search Stars

Germanium, Arsenic, and Selenium Abundances in Metal-Poor Stars*

Study of Spectral Interferences and Line Selection for Steel Analysis Using Inductively Coupled Plasma Atomic Emission Spectrometry ICP-AES

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