Atomic Transition Probabilities in Ti
                    <scp>i</scp>

Nitz, D. E.; Wickliffe, M. E.; Lawler, J. E.

doi:10.1086/313112

Cited by 36 publications

(19 citation statements)

References 13 publications

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“…Ti has five stable isotopes (Rosman & Taylor 1998) Salih & Lawler (1990) and Lawler (1991), respectively. Lawler et al (2013) have recently expanded and improved the work of Nitz et al (1998), providing accurate oscillator strengths for nearly a thousand lines by combining their FTS and eschelle BFs with the lifetimes of Salih & Lawler (1990) and Lawler (1991). Grevesse et al (1989) earlier produced accurate g f values by renormalising the relative oscillator strengths of Blackwell et al (1982aBlackwell et al ( ,b, 1983Blackwell et al ( , 1986c, which had been obtained by absorption spectroscopy in the Oxford furnace.…”

Section: Titaniummentioning

confidence: 99%

“…We prefer the data of Lawler et al (2013) where possible, but we also performed some preliminary calculations of abundances arising from lines in common between Nitz et al (1998), Blackwell-Whitehead et al (2006) Bizzarri et al (1993), and the extensive FTS and eschelle work by Wood et al (2013). The FTS study of Pickering et al (2001) also produced g f -values for many lines, where fractions for some branches were completed using theoretical oscillator strengths of weak lines from Kurucz (2011 …”

Section: Titaniummentioning

confidence: 99%

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The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

265

202

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We redetermine the abundances of all iron group nuclei in the Sun, based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model solar atmosphere, corrections for departures from local thermodynamic equilibrium (NLTE), stringent line selection procedures and high quality observational data. We have scoured the literature for the best quality oscillator strengths, hyperfine constants and isotopic separations available for our chosen lines. We find log Sc = 3.16 ± 0.04, log Ti = 4.93 ± 0.04, log V = 3.89 ± 0.08, log Cr = 5.62 ± 0.04, log Mn = 5.42 ± 0.04, log Fe = 7.47 ± 0.04, log Co = 4.93 ± 0.05 and log Ni = 6.20 ± 0.04. Our uncertainties factor in both statistical and systematic errors (the latter estimated for possible errors in the model atmospheres and NLTE line formation). The new abundances are generally in good agreement with the CI meteoritic abundances but with some notable exceptions. This analysis constitutes both a full exposition and a slight update of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data we employed.

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Section: Titaniummentioning

confidence: 99%

Section: Titaniummentioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

265

202

View full text Add to dashboard Cite

show abstract

“…For lines not measured by the Oxford group we apply values from Nitz et al (1998) and Kuehne et al (1978).…”

Section: Log Gf-values -General Commentsmentioning

confidence: 99%

Stellar abundances and ages for metal-rich Milky Way globular clusters

Feltzing¹,

Primas²,

Johnson³

2008

A&A

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Context. Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of α-elements in the clusters and the amount of α-elements is well known to influence the derivation of ages for globular clusters. Aims. We derive elemental abundances for the metal-rich globular cluster NGC 6352 and we present our methods to be used in upcoming studies of other metal-rich globular clusters. Methods. We present a study of elemental abundances for α-and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. Results. We find that NGC 6352 has [Fe/H] = −0.55, is enhanced in the α-elements to about +0.2 dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B − V) = 0.24 and (m − M) 14.05 better fits the data than the nominal values. An investigation of log g f -values for suitable Fe i lines lead us to the conclusion that the commonly used correction to the May et al. (1974) data should not be employed.

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“… (8) Grevesse, Blackwell & Petford (1989); (9) Nitz, Wickliffe & Lawler (1998); (10) Blackwell et al (1986); (11) Martin, Fuhr & Wiese (1988). …”

Section: Observationsmentioning

confidence: 99%

Intermediate-metallicity, high-velocity stars and Galactic chemical evolution

Ryan¹,

Smith²

2003

Monthly Notices of the Royal Astronomical Society

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High signal‐to‐noise ratio spectra were obtained of 10 high‐proper‐motion stars having −1 ≲[Fe/H] < 0, and a comparable number of disc stars. All but two of the high‐proper‐motion stars were confirmed to have [Fe/H] > −1.0, some approaching solar metallicity, but, even so, earlier measurements overestimated the metallicities and velocities of some of these stars. Models of stellar populations were used to assign membership probabilities to the Galactic components to which the high‐velocity stars might belong. Many were found to be more probably thick‐disc than halo objects, despite their large space motions, and two might be associated with the inner Galaxy. It may be necessary to reassess contamination of previous halo samples, such as those used to define the metallicity distribution, to account for contamination by high‐velocity thick‐disc stars, and to consider possible subcomponents of the halo. The change in [α/Fe] ratios at [Fe/H]≃−1.0 is often used to constrain the degree and timing of Type Ia supernova nucleosynthesis in Galactic chemical‐evolution models. [Ti/Fe] values were measured for eight of the high‐velocity stars. Both high‐ and low‐[Ti/Fe] halo stars exist; likewise high‐ and low‐[Ti/Fe] thick‐disc stars exist. We conclude that the [Ti/Fe]‘break’ is not well defined for a given population; nor is there a simple, continuous evolutionary sequence through the break. Implications for the interpretation of the [α/Fe] break in terms of SN Ia time‐scales and progenitors are discussed. The range of [Ti/Fe] found for high‐velocity (low rotation) thick‐disc stars contrasts with that for the low‐velocity (high rotation) thick‐disc sample studied by Prochaska et al.

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Atomic Transition Probabilities in Ti i

Cited by 36 publications

References 13 publications

The elemental composition of the Sun

The elemental composition of the Sun

Stellar abundances and ages for metal-rich Milky Way globular clusters

Intermediate-metallicity, high-velocity stars and Galactic chemical evolution

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