  Aims: We investigate the build-up of stellar mass through star formation in
field galaxies, galaxy groups, and clusters in order to better understand the
physical processes regulating star formation in different haloes.
  Methods: In order to do so we relate ongoing star formation activity to the
stellar mass by studying the integrated specific star formation rate (SSFR),
defined as the star-formation rate per unit stellar mass, as a function of
integrated stellar mass for samples of field galaxies, groups of galaxies, and
galaxy clusters at 0.18 < z < 0.85. The star formation rate (SFR) is derived
from the ultraviolet continuum for the galaxies and group members, and from
emission line fluxes for the cluster galaxies. The stellar masses are computed
from multi-band photometry including the near-infrared bands for the galaxies
and groups, and from the dynamical mass for the cluster sample.
  Results: For the first time, integrated SSFRs for clusters and groups are
presented and related to the SSFRs of field galaxies. Tentatively, we find a
continuous upper limit for galaxies, groups, and clusters in the SSFR-stellar
mass plane over seven orders of magnitude in stellar mass. This might indicate
that the physical processes which control star formation in dark matter haloes
of different mass have the same scaling with mass over a wide range of masses
from dwarf galaxies to massive clusters of galaxies.
