Chemical Abundances of the Milky Way Thick Disk and Stellar Halo. Ii. Sodium, Iron-Peak, and Neutron-Capture Elements

Ishigaki, Miho N.; Aoki, Wako; Chiba, Masashi

doi:10.1088/0004-637x/771/1/67

Cited by 166 publications

(253 citation statements)

References 139 publications

(244 reference statements)

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“…Scandium Figure 3a shows the abundance result for Sc; it is evident that the [Sc/Fe] Our results are consistent with previous works, including Prochaska et al (2000), Nissen et al (2000), Allende Prieto et al (2004), Reddy et al (2006), Brewer & Carney (2006), Adibekyan et al (2012), and Ishigaki et al (2013). It is worth noting that the sample studied in Ishigaki et al (2013) reaches [Fe/H] ≈ −3 with solar [Sc/Fe], confirming what we see from the few metal-poor stars analyzed in this work. …”

Section: General Abundance Trendssupporting

confidence: 91%

The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

Battistini

Bensby

2015

A&A

140

213

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Context. Elements heavier than Li are produced in the interiors of stars. However, for many elements the exact production sites and the timescales on which they are dispersed into the interstellar medium are unknown. Having a clear picture on the origins of the elements is important for our ability to trace and understand the formation and chemical evolution of the Milky Way and its stellar populations. Aims. The aim of this study is to investigate the origin and evolution of Sc, V, Mn, and Co for a homogeneous and statistically significant sample of stars probing the different populations of the Milky Way, in particular the thin and thick disks. Methods. Using high-resolution spectra obtained with the MIKE, FEROS, SOFIN, FIES, UVES, and HARPS spectrographs, we determine Sc, V, Mn, and Co abundances for a large sample of F and G dwarfs in the solar neighborhood. The method is based on spectral synthesis and using one-dimensional, plane-parallel, local thermodynamic equilibrium (LTE) model stellar atmospheres calculated with the MARCS 2012 code. The non-LTE (NLTE) corrections from the literature were applied to Mn and Co. Results. We find that the abundance trends derived for Sc (594 stars

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Section: General Abundance Trendssupporting

confidence: 91%

The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

Battistini

Bensby

2015

A&A

140

213

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“…7, using iron as the reference element. We compare our results with data from the literature for halo stars (François et al 2007;Ishigaki et al 2013;Nissen & Schuster 2011) and disk stars (Edvardsson et al 1993;Reddy et al 2003Reddy et al , 2006Bensby et al 2005;Nissen & Schuster 2011;Mishenina et al 2013). The halo data show a large scatter, as pointed out by François et al (2007), and the trend of element-to-Fe ratio for these four elements becomes tighter above [Fe/H] > −2.8.…”

Section: Resultsmentioning

confidence: 68%

“…All these samples together show the chemical evolution for these elements. The moderate-metallicity halo and thick-disk stars studied by Ishigaki et al (2013) show essentially solar ratios, except for a few of them, which are enhanced in La and Ba. There is also a scatter of Eu abundances and a mean overabundance of [Eu/Fe].…”

Section: Resultsmentioning

confidence: 92%

Heavy elements in old very metal-rich stars

Trevisan

Barbuy

2014

A&A

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Context. We studied a sample of high proper motion, old and metal-rich dwarf stars, selected from the NLTT catalogue. The low pericentric distances and eccentric orbits of these solar neighbourhood stars indicate that they might have originated in the inner parts of the Galaxy. Aims. Chemical tagging can probe the formation history of stellar populations. To identify the origin of a sample of 71 very metal-rich dwarf stars, we derive the abundances of the neutron-capture elements Y, Ba, La, and Eu. Methods. The spectroscopic analysis is based on optical high-resolution échelle spectra obtained with the FEROS spectrograph at the ESO 1.52 m Telescope at La Silla, Chile. The abundances of Y, Ba, La, and Eu were derived through LTE analysis, employing the MARCS model atmospheres.Results. The abundances of Y, Ba, La, and Eu vs. Fe and Mg as the reference elements indicate similarities between our sample of old metal-rich dwarf stars and the thin disk. On the other hand, the abundance ratios using O as the reference element, as well as their kinematics, suggest that our sample is clearly distinct from the thin-disk stars. They could be old inner thin-disk stars, as suggested previously, or bulge stars. In either cases, they would have migrated from the inner parts of the Galaxy to the solar neighbourhood.

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“…However, due to the increasing numerical complexity, compared with the LTE case, NLTE investigations have previously been limited to individual stars and usually only a handful of spectral lines. Contrary to the vast majority of abundance analyses available in the literature (e.g., Prochaska et al 2000;Mishenina & Kovtyukh 2001;Reddy et al 2003;Allende Prieto et al 2004;Ishigaki et al 2013), the present study will be based on NLTE line formation for Li I, C I, O I, Na I, Mg I, Al I, Si I-Si II, K I, Ca I, Sc II, Ti II, Fe I-Fe II, Cu I, Sr II, Zr II, Ba II, and Eu II. For each listed species, the original model atom was treated and tested by our previous studies (see Table 1 for details).…”

Section: Introductionmentioning

confidence: 89%

SYSTEMATIC NON-LTE STUDY OF THE −2.6 ≤ [Fe/H] ≤ 0.2 F AND G DWARFS IN THE SOLAR NEIGHBORHOOD. II. ABUNDANCE PATTERNS FROM Li TO Eu*

Zhao

Mashonkina

Yan

et al. 2016

ApJ

147

158

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For the first time, we present an extensive study of stars with individual non-LTE (NLTE) abundances for 17 chemical elements from Li to Eu in a sample of stars uniformly distributed over the −2.62 [Fe/H] +0.24 metallicity range that is suitable for the Galactic chemical evolution research. The star sample has been kinematically selected to trace the Galactic thin and thick disks and halo. We find new results and improve earlier ones as follows: (i) the element-to-iron ratios for Mg, Si, Ca, and Ti form a metal-poor (MP) plateau at a similar height of 0.3 dex, and the knee occurs at common

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Chemical Abundances of the Milky Way Thick Disk and Stellar Halo. Ii. Sodium, Iron-Peak, and Neutron-Capture Elements

Cited by 166 publications

References 139 publications

The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and Co in the Milky Way stellar disk

Heavy elements in old very metal-rich stars

SYSTEMATIC NON-LTE STUDY OF THE −2.6 ≤ [Fe/H] ≤ 0.2 F AND G DWARFS IN THE SOLAR NEIGHBORHOOD. II. ABUNDANCE PATTERNS FROM Li TO Eu*

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