Relying on samples of disk galaxies for which a detailed photometric bulge/disk decomposition has been provided in the literature, we examine the dependence of the bulge-to-disk luminosity ratio (B/D) on the blue absolute luminosity and on the environmental density. In our statistical analysis of various B/D data sets we pay particular attention to disentangling the role played by the galaxy morphologygalaxy density relation. Besides, we focus our attention on nearby (z < 0.01) galaxies, for which we can provide a three-dimensional characterization of the local galaxy density.We find that the observed tendency of galaxies to have greater B/D with increasing galaxy density simply reflects the average decline of B/D towards later morphological types together with the morphology-density relation. This relation tends to give rise also to a greater proportion of bright bulges in denser regions, because the decrease of B/D towards later types is mostly due to a dimming of the bulge rather than to a brightening of the disk. But when we remove the effect induced by the morphologydensity relation, we detect no clear evidence of a dependence of B/D on galaxy density. Furthermore, B/D turns out to be substantially unrelated to the blue absolute magnitude of the galaxy. We briefly discuss to what extent our results (partially) disagree with previous claims.
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