  The Pisces-Cetus supercluster (redshift z~0.06) is one of the richest nearby
(z<0.1) superclusters of galaxies, and emerges as a remarkable filament of
galaxies at the edges of the two-degree-field galaxy redshift survey and the
ongoing Sloan Digital Sky Survey. We explore the extent of the supercluster on
the sky and in redshift space, and map the distribution of its constituent
clusters and groups. We find evidence of enhanced star formation in galaxies
belonging to groups in the supercluster compared to those in the field. This
effect appears to be higher among the poorer groups than in the richer ones. In
contrast, star formation is suppressed in the galaxies in rich clusters, which
is consistent with previous studies. We identify two major filaments in this
supercluster, consisting of 11 and 5 Abell clusters, including Abell 133 and
Abell 85 respectively, and estimate the virial masses of the clusters from
their velocity dispersions and optical surface brightness profiles. The lower
limit to the masses of these filaments, amounting to the total virial mass of
the constituent clusters, turns out to be 5.2 x10^15, h_70^-1, M_sun and
6.0x10^15, h_70^-1, M_sun over volumes of almost 6750, h_70^-3 Mpc^3 and 19600,
h_70^-3 Mpc^3 respectively. This corresponds to mass overdensities of
Omega/Omega_crit=delta_M>4.7 and delta_M>1.3 for the two filaments making up
the supercluster.
