  Asteroid modeling efforts in the last decade resulted in a comprehensive
dataset of almost 400 convex shape models and their rotation states. This
amount already provided a deep insight into physical properties of main-belt
asteroids or large collisional families. We aim to increase the number of
asteroid shape models and rotation states. Such results are an important input
for various further studies such as analysis of asteroid physical properties in
different populations, including smaller collisional families, thermophysical
modeling, and scaling shape models by disk-resolved images, or stellar
occultation data. This provides, in combination with known masses, bulk density
estimates, but constrains also theoretical collisional and evolutional models
of the Solar System. We use all available disk-integrated optical data (i.e.,
classical dense-in-time photometry obtained from public databases and through a
large collaboration network as well as sparse-in-time individual measurements
from a few sky surveys) as an input for the convex inversion method, and derive
3D shape models of asteroids, together with their rotation periods and
orientations of rotation axes. The key ingredient is the support of more that
one hundred observers who submit their optical data to publicly available
databases. We present updated shape models for 36 asteroids, for which mass
estimates are currently available in the literature or their masses will be
most likely determined from their gravitational influence on smaller bodies,
which orbital deflection will be observed by the ESA Gaia astrometric mission.
This was achieved by using additional optical data from recent apparitions for
the shape optimization. Moreover, we also present new shape model
determinations for 250 asteroids, including 13 Hungarias and 3 near-Earth
asteroids.
