Precision measurement of relative oscillator strengths - IV. Attainment of 0.5 per cent accuracy. Fe I transitions from levels a5 D0-4 (0.00-0.12 eV)

Blackwell, D. E.; Ibbetson, P.; Petford, A. D.; Shallis, M. J.

doi:10.1093/mnras/186.3.633

Cited by 139 publications

(60 citation statements)

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“…The letters L and P are used to indicate the method used in the O'Brian work to obtain these values and stand for "lifetime" and "population method," respectively. Figure 3 shows the comparison with log ( ) gf values from Blackwell et al (1979aBlackwell et al ( , 1979bBlackwell et al ( , 1982aBlackwell et al ( , 1982b, May et al (1974), Bard & Kock (1994), and Banfield & Huber (1973). It is possible to see how log ( ) gf s from Blackwell et al agree within 1σ with our new values, which is reassuring as their experiments are considered to be the most precise by Fuhr & Wiese (2006), with uncertainties lower than 2%.…”

Section: Resultssupporting

confidence: 68%

“…A very detailed review of the situation was carried out 11 years ago by Fuhr & Wiese (2006), who presented the most comprehensive compilation of Fe I transition probabilities to date, which states clearly the need for new studies that complete and improve the quality of thousands of spectral lines in the database of Fe I log ( ) gf values. Among all the works whose values are included in Fuhr & Wiese (2006), two deserve special attention due to the quality of their results and their coverage: the experiments conducted by Blackwell et al (1979aBlackwell et al ( , 1979bBlackwell et al ( , 1980Blackwell et al ( , 1982aBlackwell et al ( , 1982bBlackwell et al ( , 1986 and O'Brian et al (1991).…”

Section: Introductionmentioning

confidence: 99%

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Fe i Oscillator Strengths for Transitions from High-lying Odd-parity Levels

Belmonte

Pickering

Ruffoni

et al. 2017

ApJ

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We report new experimental Fe I oscillator strengths obtained by combining measurements of branching fractions measured with a Fourier Transform spectrometer and time-resolved, laser-induced fluorescence lifetimes. This study covers the spectral region ranging from 213 to 1033 nm. A total of 120 experimental ( ) gf log -values coming from 15 odd-parity energy levels are provided, 22 of which have not been reported previously and 63 of which have values with lower uncertainty than the existing data. The radiative lifetimes for 60 upper energy levels are presented, 39 of which have no previous measurements.

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Section: Resultssupporting

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Fe i Oscillator Strengths for Transitions from High-lying Odd-parity Levels

Belmonte

Pickering

Ruffoni

et al. 2017

ApJ

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“…102: Bard et al (1991); Bard & Kock (1994);Blackwell et al (1979aBlackwell et al ( ,b, 1982aBlackwell et al ( ,b, 1995; O'Brian et al (1991). 114: Bridges & Kornblith (1974); Fuhr & Wiese (2006).…”

Section: Discussionmentioning

confidence: 99%

GaiaFGK benchmark stars: Metallicity

Jofré

Heiter

Soubiran

et al. 2014

A&A

252

183

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Context. To calibrate automatic pipelines that determine atmospheric parameters of stars, one needs a sample of stars, or "benchmark stars", with well-defined parameters to be used as a reference. Aims. We provide detailed documentation of the iron abundance determination of the 34 FGK-type benchmark stars that are selected to be the pillars for calibration of the one billion Gaia stars. They cover a wide range of temperatures, surface gravities, and metallicities. Methods. Up to seven different methods were used to analyze an observed spectral library of high resolutions and high signal-to-noise ratios. The metallicity was determined by assuming a value of effective temperature and surface gravity obtained from fundamental relations; that is, these parameters were known a priori and independently from the spectra. Results. We present a set of metallicity values obtained in a homogeneous way for our sample of benchmark stars. In addition to this value, we provide detailed documentation of the associated uncertainties. Finally, we report a value of the metallicity of the cool giant ψ Phe for the first time.

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“…The digit to the right of the decimal point is the ionization state ("0" = neutral, "1" = singly ionised). Gratton et al (2003); B = Oxford group including Blackwell et al (1979aBlackwell et al ( ,b, 1980Blackwell et al ( , 1986Blackwell et al ( , 1995. This table is published in its entirety in the electronic edition of the paper.…”

Section: Discussionmentioning

confidence: 99%

CNO abundances in the globular clusters NGC 1851 and NGC 6752★

Yong¹,

Grundahl²,

Norris³

2014

Monthly Notices of the Royal Astronomical Society

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We measure the C+N+O abundance sum in red giant stars in two Galactic globular clusters, NGC 1851 and NGC 6752. NGC 1851 has a split subgiant branch which could be due to different ages or C+N+O content while NGC 6752 is representative of the least complex globular clusters. For NGC 1851 and NGC 6752, we obtain average values of A(C+N+O) = 8.16 ± 0.10 (σ = 0.34) and 7.62 ± 0.02 (σ = 0.06), respectively. When taking into account the measurement errors, we find a constant C+N+O abundance sum in NGC 6752. The C+N+O abundance dispersion is only 0.06 dex, and such a result requires that the source of the light element abundance variations does not increase the C+N+O sum in this cluster. For NGC 1851, we confirm a large spread in C+N+O. In this cluster, the anomalous RGB has a higher C+N+O content than the canonical RGB by a factor of four (∼0.6 dex). This result lends further support to the idea that the two subgiant branches in NGC 1851 are roughly coeval, but with different CNO abundances.

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Precision measurement of relative oscillator strengths - IV. Attainment of 0.5 per cent accuracy. Fe I transitions from levels a5 D0-4 (0.00-0.12 eV)

Cited by 139 publications

References 0 publications

Fe i Oscillator Strengths for Transitions from High-lying Odd-parity Levels

Fe i Oscillator Strengths for Transitions from High-lying Odd-parity Levels

GaiaFGK benchmark stars: Metallicity

CNO abundances in the globular clusters NGC 1851 and NGC 6752★

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