  We have analysed, for the first time, the clustering properties of Wolf-Rayet
(W-R) galaxies, using a large sample of 846 W-R galaxies selected from the Data
Release 4 (DR4) of the SDSS. We compute the cross-correlation function between
W-R galaxies and a reference sample of galaxies drawn from the DR4. We compare
the function to the results for control samples of non-W-R star-forming
galaxies that are matched closely in redshift, luminosity, concentration,
4000-\AA break strength and specific star formation rate (SSFR). On scales
larger than a few Mpc, W-R galaxies have almost the same clustering amplitude
as the control samples, indicating that W-R galaxies and non-W-R control
galaxies populate dark matter haloes of similar masses. On scales between
0.1--1$h^{-1}$ Mpc, W-R galaxies are less clustered than the control samples,
and the size of the difference depends on the SSFR. Based on both observational
and theoretical considerations, we speculate that this negative bias can be
interpreted by W-R galaxies residing preferentially at the centers of their
dark matter haloes. We examine the distribution of W-R galaxies more closely
using the SDSS galaxy group catalogue of Yang et al., and find that $\sim$82%
of our W-R galaxies are the central galaxies of groups, compared to $\sim$74%
for the corresponding control galaxies. We find that W-R galaxies are hosted,
on average, by dark matter haloes of masses of$10^{12.3}M_\odot$, compared to
$10^{12.1}M_\odot$ for centrally-located W-R galaxies and $10^{12.7}M_\odot$
for satellite ones. We would like to point out that this finding, which
provides a direct observational support to our conjecture, is really very crude
due to the small number of W-R galaxies and the incompleteness of the group
catalogue, and needs more work in future with larger samples.
