  The cosmological curvature perturbation may be generated when some `curvaton'
field, different from the inflaton, oscillates in a background of unperturbed
radiation. In its simplest form the curvaton paradigm requires the Hubble
parameter during inflation to be bigger than $10^7\GeV$, but this bound may be
evaded if the curvaton field (or an associated tachyon) is strongly coupled to
a field which acquires a large value at the end of inflation. As a result the
curvaton paradigm might be useful in improving the viability of low-scale
inflation models, in which the supersymmetry-breaking mechanism is the same as
the one which operates in the vacuum.
