  We present first results from an on-going survey of the stellar populations
of the bulges and inner disks of spirals at various points along the Hubble
sequence. In particular, we are investigating the hypotheses that bulges of
early-type spirals are akin to (and may in fact originally have been)
intermediate-luminosity ellipticals while bulges of late-type spirals are
formed from dynamical instabilities in their disks. Absorption-line
spectroscopy of the central regions of Sa--Sd spirals is combined with stellar
population models to determine integrated mean ages and metallicities. These
ages and metallicities are used to investigate stellar population differences
both between the bulges and inner disks of these spirals and between bulges and
ellipticals in an attempt to place observational constraints on the formation
mechanisms of spiral bulges.
