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We present the analysis of the radial gradients of stellar absorption linesin a sample of 32 bulges of edge-on spiral galaxies, spanning nearly the fullHubble sequence (from S0 to Sc types), and a large range of velocity dispersion(from about 60 to 300 km/s). Different diagnostics such as index-index,gradient-gradient diagrams, and simple stellar population models are used totackle the origin of the variation of the bulge stellar population. We findthat the vast majority of bulges show older age, lower metallicity and higher[alpha/Fe] in their outer regions than in their central parts. The radialgradients in [Fe/H] are 2 to 3 times larger than in Log(age). The relationbetween gradient and bulge velocity dispersion is interpreted as a gradualbuild up of the gradient mean values and their dispersions from high to lowvelocity dispersion, rather than a pure correlation. The bulge effective radiiand the Hubble type of the parent galaxies seem to play a more minor role incausing the observed spatial distributions. At a given velocity dispersion,bulges and ellipticals share common properties.

Stellar Population Gradients in Bulges along the Hubble Sequence: II. Relations with Galaxy Properties