  We consider the multiplicity of stellar systems with (combined) magnitude
brighter than 6.00 in Hipparcos magnitudes. We identify 4559 such bright
systems (including the Sun), and the frequencies of multiplicities 1, 2,..., 7
are found to be 2718, 1437, 285, 86, 20, 11 and 2. We discuss the
uncertainties, which are substantial. We also consider the distributions of
periods of orbits and sub-orbits. We note that for the even more restricted set
of 478 systems with V_H <= 4.00 the proportions of higher multiples up to
sextuple are progressively larger (213, 179, 54, 19, 8, 5), suggesting
substantial incompleteness in even the reasonably well-studied larger sample.
  This sample can be seen as relatively thoroughly studied for multiplicity,
and reasonably representative of stars more massive than the Sun. But the
restriction to V_H <= 6 means that our sample contains hardly any systems where
all components are low-mass main-sequence stars (K or M).
  Data on multiplicity is important as a constraint on (a) the star-formation
problem, (b) the problem of the evolution of the Galactic stellar population,
and (c) the interaction of dynamics and evolution through the effect of Kozai
cycles. We discuss these topics briefly.
