How spectral fittings of stellar clusters are affected by the wavelength range used
Star clusters (SCs) are excellent laboratories to test stellar populations, as well as to determine their key properties such as age (t) and metallicity ([Fe/H]). For distant (extragalactic) SCs only integrated spectra are available, and one of the most powerful methods to study these properties is...
Guardado en:
| Autores principales: | , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2024
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/171231 |
| Aporte de: |
| Sumario: | Star clusters (SCs) are excellent laboratories to test stellar populations, as well as to determine their key properties such as age (t) and metallicity ([Fe/H]). For distant (extragalactic) SCs only integrated spectra are available, and one of the most powerful methods to study these properties is through synthesis modeling. Although this method is very useful, there are several limitations in the results of the models based on spectral synthesis. Here we apply this technique to spectra of Large Magellanic Cloud Star Clusters for different spectral coverage using the synthesis code Starlight, in order to explore the dependence of the stellar population parameters with the wavelength ranges used. |
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