  The consistency of planet formation models suffers from the disconnection
between the regime of small and large bodies. This is primarily caused by
so-called growth barriers: the direct growth of larger bodies is halted at
centimetre-sized objects and particular conditions are required for the
formation of larger, gravitationally bound planetesimals. We aim to connect
models of dust evolution and planetesimal formation to identify regions of
protoplanetary discs that are favourable for the formation of kilometre-sized
bodies and the first planetary embryos. We combine semi-analytical models of
viscous protoplanetary disc evolution, dust growth and drift including
backreaction of the dust particles on the gas, and planetesimal formation via
the streaming instability into one numerical code. We investigate how
planetesimal formation is affected by the mass of the protoplanetary disc, its
initial dust content, and the stickiness of dust aggregates. We find that the
dust growth and drift leads to a global redistribution of solids. The pile-up
of pebbles in the inner disc provides local conditions where the streaming
instability is effective. Planetesimals form in an annulus with its inner edge
lying between 0.3 AU and 1 AU and its width ranging from 0.3 AU to 3 AU. The
resulting surface density of planetesimals follows a radial profile that is
much steeper than the initial disc profile. These results support formation of
terrestrial planets in the solar system from a narrow annulus of planetesimals,
which reproduces their peculiar mass ratios.
