  The available set of spin and shape modelled asteroids is strongly biased
against slowly rotating targets and those with low lightcurve amplitudes. As a
consequence of these selection effects, the current picture of asteroid spin
axis distribution, rotation rates, or radiometric properties, might be affected
too.
  To counteract these selection effects, we are running a photometric campaign
of a large sample of main belt asteroids omitted in most previous studies. We
determined synodic rotation periods and verified previous determinations. When
a dataset for a given target was sufficiently large and varied, we performed
spin and shape modelling with two different methods.
  We used the convex inversion method and the non-convex SAGE algorithm,
applied on the same datasets of dense lightcurves. Unlike convex inversion, the
SAGE method allows for the existence of valleys and indentations on the shapes
based only on lightcurves.
  We obtained detailed spin and shape models for the first five targets of our
sample: (159) Aemilia, (227) Philosophia, (329) Svea, (478) Tergeste, and (487)
Venetia. When compared to stellar occultation chords, our models obtained an
absolute size scale and major topographic features of the shape models were
also confirmed. When applied to thermophysical modelling, they provided a very
good fit to the infrared data and allowed their size, albedo, and thermal
inertia to be determined.
  Convex and non-convex shape models provide comparable fits to lightcurves.
However, some non-convex models fit notably better to stellar occultation
chords and to infrared data in sophisticated thermophysical modelling (TPM). In
some cases TPM showed strong preference for one of the spin and shape
solutions. Also, we confirmed that slowly rotating asteroids tend to have
higher-than-average values of thermal inertia.
