Table 3.
Gradients along the cut #2 (Fig. 8) perpendicular to the major axis, i.e. at 2/3 × barlength distance from the centre.
| Galaxy | Δ AgeLW, L | Δ AgeLW, T | Δ AgeMW, L | Δ AgeMW, T | Δ [Z/H]LW, L | Δ [Z/H]LW, T | Δ [Z/H]MW, L | Δ [Z/H]MW, T |
|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| IC 1438 | −0.65 ± 0.38 | −0.77 ± 0.15 | 0.48 ± 0.18 | 0.09 ± 0.25 | −0.12 ± 0.07 | −0.14 ± 0.03 | 0.01 ± 0.02 | −0.04 ± 0.01 |
| NGC 4303 | −1.00 ± 0.16 | 0.04 ± 0.39 | 0.72 ± 0.27 | 0.32 ± 0.41 | 0.03 ± 0.06 | −0.01 ± 0.06 | 0.11 ± 0.02 | 0.03 ± 0.06 |
| NGC 4371 ( † ) | −0.66 ± 0.06 | −0.50 ± 0.08 | −0.29 ± 0.07 | −0.18 ± 0.05 | −0.01 ± 0.01 | −0.01 ± 0.01 | 0.00 ± 0.01 | −0.00 ± 0.01 |
| NGC 4643 ( † ) | 0.06 ± 0.05 | 0.33 ± 0.12 | 0.11 ± 0.05 | 0.34 ± 0.09 | −0.10 ± 0.02 | −0.10 ± 0.01 | −0.08 ± 0.02 | −0.06 ± 0.01 |
| NGC 4981 | −0.64 ± 0.11 | −0.38 ± 0.50 | 1.20 ± 0.26 | 0.67 ± 0.29 | −0.08 ± 0.04 | −0.02 ± 0.04 | 0.09 ± 0.06 | 0.07 ± 0.04 |
| NGC 4984 | −0.30 ± 0.05 | −0.44 ± 0.12 | 0.31 ± 0.12 | 0.22 ± 0.13 | −0.01 ± 0.02 | 0.00 ± 0.02 | 0.02 ± 0.02 | 0.02 ± 0.02 |
| NGC 5248 ( ⋆ ) | 0.37 ± 0.21 | −1.06 ± 0.68 | −0.02 ± 0.37 | −0.00 ± 0.38 | 0.03 ± 0.03 | −0.07 ± 0.03 | −0.01 ± 0.04 | −0.08 ± 0.04 |
| NGC 6902 | −1.20 ± 0.26 | −0.73 ± 0.15 | 0.07 ± 0.10 | 0.38 ± 0.10 | −0.02 ± 0.01 | −0.03 ± 0.01 | 0.03 ± 0.01 | 0.02 ± 0.02 |
| NGC 7755 | −0.35 ± 0.22 | −0.29 ± 0.39 | 0.35 ± 0.22 | 0.22 ± 0.34 | −0.10 ± 0.03 | −0.08 ± 0.02 | −0.02 ± 0.05 | −0.03 ± 0.03 |
| Mean | −0.69 ± 0.32 | −0.43 ± 0.27 | 0.52 ± 0.36 | 0.32 ± 0.18 | −0.05 ± 0.05 | −0.05 ± 0.05 | 0.04 ± 0.04 | 0.01 ± 0.04 |
Notes. Column (1) gives the name of the galaxy; Cols. (2)−(5) show the gradients of mean ages divided into light-weighted (LW) and mass-weighted (MW) values, as well as into the gradients along the leading edge of the bar (L) and the trailing edge (T); Cols. (6)−(10) show the gradients of mean metallicities in the same format as for the ages. The last row shows the mean values from all galaxies except NGC 4371, NGC 4643, and NGC 5248, and the standard deviation between individual objects. The standard deviation of the mean is higher than the propagated error of the individual objects. ( † )For NGC 4371 and NGC 4643, we were unable to define the sense of rotation. For these galaxies, the sides (L/T) were arbitrarily chosen. ( ⋆ )NGC 5248 is a clear outlier and was not included in the calculation of the means.
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