  We investigate the dependence of galaxy clustering on luminosity and spectral
type using the 2dF Galaxy Redshift Survey (2dFGRS). Spectral types are assigned
using the principal component analysis of Madgwick et al. We divide the sample
into two broad spectral classes: galaxies with strong emission lines
(`late-types'), and more quiescent galaxies (`early-types'). We measure the
clustering in real space, free from any distortion of the clustering pattern
due to peculiar velocities, for a series of volume-limited samples. The
projected correlation functions of both spectral types are well described by a
power law for transverse separations in the range 2 < (sigma/Mpc/h) < 15, with
a marginally steeper slope for early-types than late-types. Both early and late
types have approximately the same dependence of clustering strength on
luminosity, with the clustering amplitude increasing by a factor of ~2.5
between L* and 4 L*. At all luminosities, however, the correlation function
amplitude for the early-types is ~50% higher than that of the late-types. These
results support the view that luminosity, and not type, is the dominant factor
in determining how the clustering strength of the whole galaxy population
varies with luminosity.
