Atmospheric parameters and chemical abundances within 100 pc. A sample of G, K, and M main-sequence stars
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| Format: | Preprint |
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2024
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| author | López-Valdivia, Ricardo Adame, Lucía Lagunas, Eduardo Zagala Román-Zúñiga, Carlos G. Hernández, Jesús Sánchez, Edilberto Fernández-Trincado, José G. Carigi, Leticia Kounkel, Marina Lane, Richard R. Stassun, Keivan G. Villanova, Sandro |
| author_facet | López-Valdivia, Ricardo Adame, Lucía Lagunas, Eduardo Zagala Román-Zúñiga, Carlos G. Hernández, Jesús Sánchez, Edilberto Fernández-Trincado, José G. Carigi, Leticia Kounkel, Marina Lane, Richard R. Stassun, Keivan G. Villanova, Sandro |
| contents | 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 disk main-sequence stars in the 100 pc solar neighborhood, 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 Teff, 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 color-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 centered around slightly sub-solar values, in agreement with previous results for the solar neighborhood. The over 1600 main-sequence stars atmospheric parameters and chemical abundances presented here are useful in follow-up studies of the solar neighborhood or as a training set for data-driven methods. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_17640 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Atmospheric parameters and chemical abundances within 100 pc. A sample of G, K, and M main-sequence stars López-Valdivia, Ricardo Adame, Lucía Lagunas, Eduardo Zagala Román-Zúñiga, Carlos G. Hernández, Jesús Sánchez, Edilberto Fernández-Trincado, José G. Carigi, Leticia Kounkel, Marina Lane, Richard R. Stassun, Keivan G. Villanova, Sandro Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies 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 disk main-sequence stars in the 100 pc solar neighborhood, 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 Teff, 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 color-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 centered around slightly sub-solar values, in agreement with previous results for the solar neighborhood. The over 1600 main-sequence stars atmospheric parameters and chemical abundances presented here are useful in follow-up studies of the solar neighborhood or as a training set for data-driven methods. |
| title | Atmospheric parameters and chemical abundances within 100 pc. A sample of G, K, and M main-sequence stars |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.17640 |