A standard stellar library for evolutionary synthesis

Free access article

Issue		Astron. Astrophys. Suppl. Ser. Volume 130, Number 1, May_II 1998


Page(s)		65 - 75
DOI		http://dx.doi.org/10.1051/aas:1998405

DOI: 10.1051/aas:1998405

Astron. Astrophys. Suppl. Ser. 130, 65-75

II. The M dwarf extension

T. Lejeune ^1,2 - F. Cuisinier ³ - R. Buser ¹

Send offprint request: T. Lejeune - lejeune@astro.unibas.ch

1 - Astronomisches Institut der Universität Basel, Venusstr. 7, CH-4102 Binningen, Switzerland
2 - Observatoire de Strasbourg, 11 rue de l'Université, F-67000 Strasbourg, France
3 - Universidade de São Paulo, IAG, Dept. de Astronomia, C.P. 9638, São Paulo 01065-970, Brasil

Received May 23; accepted October 31, 1997

Abstract:

A standard library of theoretical stellar spectra intended for multiple synthetic photometry applications including spectral evolutionary synthesis is presented. The grid includes M dwarf model spectra, hence complementing the first library version established in Paper I ([Lejeune et al. 1997]). It covers wide ranges of fundamental parameters: $T_{\mathrm{eff}}$ : 50000 K $\sim$ 2000 K, $\log g$ : 5.5 $\sim -1.02$ , and [M/H]: $+1.0 \sim -5.0$ . A correction procedure is also applied to the theoretical spectra in order to provide color-calibrated flux distributions over a large domain of effective temperatures. For this purpose, empirical $T_{\mathrm{eff}}$ -color calibrations are constructed between 11500 K and 2000 K, and semi-empirical calibrations for non-solar abundances ([M/H] = -3.5 to +1.0) are established. Model colors and bolometric corrections for both the original and the corrected spectra, synthesized in the $(UBV)_{\rm J}(RI)_{\rm C}JHKLL'M$ system, are given for the full range of stellar parameters. We find that the corrected spectra provide a more realistic representation of empirical stellar colors, though the method employed is not completely adapted to the lowest temperature models. In particular the original differential colors of the grid implied by metallicity and/or luminosity changes are not preserved below 2500 K. Limitations of the correction method used are also discussed.

Key words: stars: fundamental parameters -- stars: late type

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