Chemical abundances for a sample of FGK dwarfs in the Pleiades open cluster from APOGEE

被引：2

作者：

Grilo, Vinicius ^{[1
]}

Souto, Diogo ^{[1
]}

Cunha, Katia ^{[2
,3
]}

Guerco, Rafael ^{[2
,4
]}

Vieira, Rodrigo ^{[1
]}

Smith, Verne ^{[5
]}

Vilar, Deusalete ^{[1
]}

Silva-Andrade, Anderson ^{[1
]}

Wanderley, Fabio ^{[2
]}

Daflon, Simone ^{[2
]}

Silva, Joao Victor Sales ^{[2
]}

机构：

[1] Univ Fed Sergipe, Dept Fis, Av Marcelo Deda Chagas,S-N, BR-49107230 Sao Cristovao, SE, Brazil

[2] MCTIC, Observ Nacl, R Gen Jose Cristino,77, BR-20921400 Rio De Janeiro, Brazil

[3] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

[4] Univ Catolica Norte, Inst Astron, Av Angamos 0610, Antofagasta, Chile

[5] NSFs NOIRLab, 950 North Cherry Ave, Tucson, AZ 85719 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 534卷 / 04期

基金：

美国安德鲁·梅隆基金会; 美国国家科学基金会;

关键词：

stars: abundances; stars: fundamental parameters; infrared: stars; RED SUPERGIANT STARS; GALACTIC METALLICITY GRADIENT; ATOMIC DIFFUSION; OLD STARS; DATA RELEASE; STELLAR CHARACTERIZATION; MAIN-SEQUENCE; MESA ISOCHRONES; COMA BERENICES; GIANT STARS;

D O I：

10.1093/mnras/stae2209

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This paper presents chemical abundances of 12 elements (C, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe) for 80 FGK dwarfs in the Pleiades open cluster, which span a temperature range of similar to 2000 K in Teff, using the high-resolution (R similar to 22 500) near-infrared SDSS (Sloan Digital Sky Survey)-IV/APOGEE (Apache Point Observatory Galactic Evolution Experiment) spectra (lambda 1.51-1.69 mu m). Using a 1D local thermodynamic equilibrium abundance analysis, we determine an overall metallicity of [Fe/H] = +0.03 +/- 0.04 dex, with the elemental ratios [alpha/Fe] = +0.01 +/- 0.05, [odd-z/Fe] = -0.04 +/- 0.08, and [iron peak/Fe] = -0.02 +/- 0.08. These abundances for the Pleiades are in line with the abundances of other open clusters at similar galactocentric distances as presented in the literature. Examination of the abundances derived from each individual spectral line revealed that several of the stronger lines displayed trends of decreasing abundance with decreasing Teff. The list of spectral lines that yield abundances that are independent of Teff are presented and used for deriving the final abundances. An investigation into possible causes of the temperature-dependent abundances derived from the stronger lines suggests that the radiative codes and the APOGEE line list we employ may inadequately model van der Waals broadening, in particular in the cooler K dwarfs

引用

页码：3005 / 3021

页数：17

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