  It is currently impossible to determine the abundances of stellar populations
star-by-star in dense stellar systems more distant than a few megaparsecs.
Therefore, methods to analyse the composite light of stellar systems are
required. I review recent progress in determining the abundances and abundance
ratios of early-type galaxies. I begin with `direct' abundance measurements:
colour--magnitude diagrams of and planetary nebula in nearby early-type
galaxies. I then give an overview of `indirect' abundance measurements:
inferences from stellar population models, with an emphasis on cross-checks
with `direct' methods. I explore the variations of early-type galaxy abundances
as a function of mass, age, and environment in the local Universe. I conclude
with a list of continuing difficulties in the modelling that complicate the
interpretation of integrated spectra and I look ahead to new methods and new
observations.
