  We consider a weighted biasing scheme for galaxy clustering. This differs
from previous treatments in the fact that the biased density field coincides
with the background mass--density whenever the latter exceeds a given threshold
value. There is some physical motivation for this scheme and it is in better
accord with intuitive ideas than models based on the Kaiser (1984) analysis of
the clustering of rich clusters. We explain how different classes of object
could be biased in different ways with respect to the underlying density
distribution but still have $b=1$. We also show that if one applies our scheme
consistently a weak dependence of $b$ upon density can be implied. This could
also be the reason why the correlation function of galaxies in groups does not
differ substantially from the correlation function of all galaxies.
