Calibration of (B–V)0 for MILES stars

A. de C. Milone1*, P. Sánchez-Blázquez4, A. Vazdekis2,3, C. Allende Prieto2,3, A. Sansom5
1Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758, 12227-010, S. J. Campos, Brazil
2Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38205, La Laguna, Tenerife, Spain
3Depto. de Astrofísica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain
4Depto. de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco 28409, Madrid, Spain
5Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UK

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Abstract

The integrated spectral properties of a stellar system bring information from the mixture of stellar populations within the system. The (B–V) colour is one of the observational properties that can help determine the age and metallicity of stellar populations in a star cluster or even in galaxies. We have derived a series of empirical calibrations of the intrinsic colour, (B–V)0, as a function of Teff, [Fe/H] and [µ/Fe]. The stellar parameters of MILES stars have been redetermined homogeneously. The calibrations were obtained individually for distinct spectral types (O-B, A, F-G-K and M), which were then further subdivided into as many as five ranges in [Fe/H]. For the M types only, the stars were divided into dwarfs and giants. (B–V)0 was measured directly using the MILES fully calibrated stellar spectra (typical error = 0.025 mag). Here, we present just the (B–V)0 calibrations for F-G-K types that are split into five [Fe/H] ranges. We find that the error in (B–V)0 varies from 0.014–0.022 mag. The next main goal is to compute (B–V)0 self-consistently for semi-empirical simple stellar population models based on MILES.



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Keywords : catalogues – stars: fundamental parameters – stars: abundances