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Fig. 3


Left: point density diagram of the equivalent width of the Hα nebular emission, WHα, versus the light fraction due to populations younger than 32 Myr (xY) for 12 540 radial bins of 416 galaxies. The color bar shows the density of data points on a logarithmic scale. White circles trace the mean relation (obtained from the mean WHα values in xY-bins). The gray line shows the linear fit to all points: WHα(Å) = 1.024 + 1.208 xY(%). Horizontal lines are drawn at WHα = 3 (dashed) and 6 Å (dotted). Vertical lines mark xY = 3.4% (the mean xY for points with WHα< 3 Å; dashed) and xY = 4.3% (the mean xY for points with WHα< 6 Å; dotted). Middle: mean WHα radial profiles for galaxies in the seven Hubble type bins. Horizontal lines indicate WHα = 3 (dashed), and 6 Å (dotted). Right: radial profile of xY in the same Hubble type groups. Horizontal lines indicate xY = 3.4 (dashed) and 4.3% (dotted). The dispersion in WHα (middle panel) and xY (right panel) measured at 1 HLR in Sb galaxies is shown as an error bar. (The corresponding statistical errors are much smaller.)

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