All Tables

Table 1: Coefficients to estimate the expected random error in typical line-strength indices and colors, as a function of the mean signal-to-noise ratio per Å, following Eq. (3). Note that these coefficients are valid for atomic indices when measured in magnitudes (i.e. as if they were molecular indices). For line-strength indices measured in Å see coefficients in Table 1 in Cardiel et al. (1998).
Table 2: Logarithm of the suitability index, $\log[\kappa]$ , - see Eq. (21) - for the study of the age-metallicity degeneracy, computed for different combinations of common line-strength indices in the optical range. For the generation of these numbers we have employed the predictions of Bruzual & Charlot (2001) models, for single stellar populations of 12 Gyr old and solar metallicity. Better diagrams are those for which $\kappa$ are lower. In this sense, and as a guide for the eye, we have boldfaced and underlined the 10% of these numbers with the lowest values.
Table 3: Same than Table 2 but for different combinations of colors.
Table 4: Same than Table 2 but for different combinations of line-strength indices and colors.
Table 5: H $\gamma _{{\rm VA},\sigma }$ correspond to the $[\mbox{H}\gamma+1/2(\mbox{Fe~{\sc i}}+\mbox{Mg~{\sc i}})]_\sigma$ indices defined by Vazdekis & Arimoto (1999). Model references are W94: Worthey (1994); JW95: Jones & Worthey (1995); WO97: Worthey & Ottaviani (1997); and V99: Vazdekis & Arimoto (1999).
Table 6: Numerical values for the example of Sect. 4.2 (see also Fig. 2). The upper table lists the input line-strength indices employed in the computation of the bivariate polynomial transformations in Figs. 2a, c around the model predictions for a SSP of 12 Gyr with solar metallicity (boldfaced). The lower table displays the different parameters involved in the calculation of the previous transformations, and the factors leading to the suitability index in Eq. (21).
Table 7: Comparison of $\log[\kappa]$ for the study of the age-metallicity degeneracy, computed from the prediction of three sets of models, W94 (Worthey 1994), V00 (Vazdekis et al. 1996; Blakeslee et al. 2001), and BC01 (Bruzual & Charlot 2001). In all the cases we have derived the suitability parameters for SSP around 12 Gyr old and solar metallicity.
Table B.1: Numerical values of the $\xi$ coefficients computed from Eq. (B.13), for a set of common photometric bands corresponding to the filters given in Table 9 of Fukugita et al. (1995). Filter widths were determined with Eq. (B.20).