Atmospheric parameters and chemical abundances within 100 pc: a sample of G, K, and M main-sequence stars

被引:0
作者
Lopez-Valdivia, Ricardo [1 ]
Adame, Lucia [1 ]
Lagunas, Eduardo Zagala [2 ]
Roman-Zuniga, Carlos G. [1 ]
Hernandez, Jesus [1 ]
Sanchez, Edilberto [1 ]
Fernandez-Trincado, Jose G. [3 ]
Carigi, Leticia [4 ]
Kounkel, Marina [5 ]
Lane, Richard R. [6 ]
Stassun, Keivan G. [7 ]
Villanova, Sandro [8 ]
机构
[1] Univ Nacl Autonoma Mexico, Inst Astron, AP 106, Ensenada 22800, BC, Mexico
[2] Univ Autonoma Baja Calif, Fac Ciencias, Ensenada 22860, BC, Mexico
[3] Univ Catolica Norte, Inst Astron, Av Angamos 0610, Antofagasta, Chile
[4] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, Mexico
[5] Univ North Florida, Dept Phys & Astron, 1 UNF Dr, Jacksonville, FL 32224 USA
[6] Univ Bernardo OHiggins, Ctr Invest Astron, Ave Viel 1497, Santiago, Chile
[7] Vanderbilt Univ, Dept Phys & Astron, VU Stn 1807, Nashville, TN 37235 USA
[8] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile
基金
美国安德鲁·梅隆基金会;
关键词
stars: abundances; stars: fundamental parameters; stars: solar-type - techniques: spectroscopic; PARSEC EVOLUTIONARY TRACKS; PLANET SEARCH PROGRAM; SOLAR NEIGHBORHOOD; MASSIVE STARS; LINE LISTS; APOGEE NET; STELLAR; TELESCOPE; MODEL; TEMPERATURES;
D O I
10.1093/mnras/stae1809
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
To date, we have access to enormous inventories of stellar spectra that allow the extraction of atmospheric parameters and chemical abundances essential in stellar studies. However, characterizing such a large amount of data is complex and requires a good understanding of the studied object to ensure reliable and homogeneous results. In this study, we present a methodology to measure homogenously the basic atmospheric parameters and detailed chemical abundances of over 1600 thin disc main-sequence stars in the 100 pc solar neighbourhood, using APOGEE-2 infrared spectra. We employed the code tonalli to determine the atmospheric parameters using a prior on log g. The log g prior in tonalli implies an understanding of the treated population and helps to find physically coherent answers. Our atmospheric parameters agree within the typical uncertainties (100 K in T-eff, 0.15 dex in log g and [M/H]) with previous estimations of ASPCAP and Gaia DR3. We use our temperatures to determine a new infrared colour-temperature sequence, in good agreement with previous works, that can be used for any main-sequence star. Additionally, we used the bacchus code to determine the abundances of Mg, Al, Si, Ca, and Fe in our sample. The five elements (Mg, Al, Si, Ca, Fe) studied have an abundance distribution centred around slightly subsolar values in agreement with previous results for the solar neighbourhood. The over 1600 main-sequence stars' atmospheric parameters and chemical abundances presented here are useful in follow-up studies of the solar neighbourhood or as a training set for data-driven methods.
引用
收藏
页码:395 / 412
页数:18
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