All Tables

Table 1: Velocity dispersion and line-strength gradients for the sample of 82 galaxies. A portion of the table is shown for guidance regarding its form and content. For each galaxy and index, the first line shows the measured gradient, while the second row lists its corresponding formal error. The full table is available in electronic form at http://www.edpsciences.org.
Table 3: Mean gradients of age, [M/H], and metallicity, derived with different indices for LDEGs. $\sigma$ : typical deviation; N: number of galaxies; $N_{\rm eff}$ : effective number of points, $N_{\rm eff}=\left [\sum (1/\sigma ^2)\right ]^2$ / $\sum \left [(1/\sigma ^2)^2\right ]$ ; t: t-statistic to check the hypothesis "mean $\ne$ 0''; $\sigma _{\rm exp}$ : typical deviation expected from errors; $\alpha$ : level of significance to reject the hypothesis " $\sigma =\sigma _{\rm exp}$ ''. The last column contains the t-statistic used to test the hypothesis "mean grad[M/H] = mean grad[M/H]'' (with different indices).
Table 4: Linear fits and probability of no correlation between the metallicity gradient and the gradient of velocity dispersion. N: number of galaxies in the fit; $b+\sigma (b)$ : slope and error of the linear fit (the errors have been calculated by Monte Carlo simulations, as described in the text); t: t-statistic to verify the hypothesis "b=0'' (a t value higher than 1.96 allows the hypothesis to be rejected, with a significance level lower than 0.05); Pnc: probability of no correlation in a non-parametric Spearman test.
Table 5: Correlation between the gradients of age and metallicity and the central velocity dispersion. The brackets show the different indicators used to calculate the metallicity gradients. The first and the second rows refer to the values calculated using the ten indicators described in Sect. 3. t: t-parameter calculated as the quotient of the slope and its error, computed through Monte Carlo simulations; Pnc: probability of no correlation according to a non-parametric Spearman test.
Table 6: Parameters of the linear fits, weighted with errors, of the age and metallicities (measured in different index-index diagrams indicated between brackets) and the central velocity dispersion. The table shows the results for the central values ( $a_{\rm c}$ and $b_{\rm c}$ ) and for the global values ( $a_{\rm g}$ and $b_{\rm g}$ ). The coefficients a and b represent the zero point and the slope of the linear fit, respectively. The last column shows the t parameter obtained in a t-test to check the hypothesis $b_{\rm c}=b_{\rm g}$ . A value of t higher than 2.326 allows us to reject the hypothesis with a significance level lower than 0.01.
Table 7: Mean stellar population gradients and their errors for HDEGs. $\sigma$ : standard deviation about the mean; N: number of galaxies averaged; $N_{\rm eff}$ : effective number of points; t: t-statistic to verify the hypothesis "mean = 0''; $\sigma _{\rm exp}$ : standard deviation expected from the errors; $\alpha$ : significance level to reject the hypothesis " $\sigma$ = $\sigma _{\rm exp}$ '' in a $\chi ^2$ test. Column 9 shows the t-statistic to confirm whether the gradients obtained with individual indicators are the same as the metallicity gradients obtained with a combination of ten different indicators. As a reference, the 10th column shows the mean gradients obtained for the LDEGs from Sect. 4 (see Table 3). The final column of the table shows the t-statistic, to verify if the mean gradients are the same for both samples of galaxies, LDEGs and HDEGs. A high value of t indicates significant differences.
Full version
Table 1: Velocity dispersion and line-strength gradients for the sample of 82 galaxies. A portion of the table is shown for guidance regarding its form and content. For each galaxy and index, the first line shows the measured gradient, while the second row lists its corresponding formal error. The full table is available in the electronic edition of this paper.
Table 2: Age and metallicity gradients derived with the method of Sect. 3 (second and third columns), and metallicity gradients derived in several index-index diagrams using different metallicity indicators (as indicated in the column headers) combined with H $\beta$ . The second row for each galaxy indicates the associated errors in the gradients.