Stellar physics with the ALHAMBRA photometric system

The ALHAMBRA photometric system was specifically designed to perform a tomography of the Universe in some selected areas. Although mainly designed for extragalactic purposes, its 20 contiguous, equal-width, medium-band photometric system in the optical wavelength range, shows a great capacity for st...

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Detalhes bibliográficos
Autores: Villegas, Aparicio, Alfaro, E. J., Cabrera-Caño, J., Moles, M., Benítez, N., Perea, J., del Olmo, A., Fernánez-Soto, A., Cristóbal-Hornillos, D., Aguerri, J. A. L.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2011
País:Chile
Idioma:inglés
OAI Identifier:oai:repositorio.anid.cl:10533/245895
Acesso em linha:https://hdl.handle.net/10533/245895
Access Level:acceso abierto
Descrição
Resumo:The ALHAMBRA photometric system was specifically designed to perform a tomography of the Universe in some selected areas. Although mainly designed for extragalactic purposes, its 20 contiguous, equal-width, medium-band photometric system in the optical wavelength range, shows a great capacity for stellar classification. In this contribution we propose a methodology for stellar classification and physical parameter estimation (Teff, log g, [Fe/H], and color excess E(B - V)) based on 18 independent reddening-free Q-values from the ALHAMBRA photometry. Based on the theoretical Spectral library BaSeL 2.2, and applied to 288 stars from the Next Generation spectral Library (NGSL), we discuss the reliability of the method and its dependence on the extinction law used.

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