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Asteroid modeling efforts in the last decade resulted in a comprehensivedataset of almost 400 convex shape models and their rotation states. Thisamount already provided a deep insight into physical properties of main-beltasteroids or large collisional families. We aim to increase the number ofasteroid shape models and rotation states. Such results are an important inputfor various further studies such as analysis of asteroid physical properties indifferent populations, including smaller collisional families, thermophysicalmodeling, and scaling shape models by disk-resolved images, or stellaroccultation data. This provides, in combination with known masses, bulk densityestimates, but constrains also theoretical collisional and evolutional modelsof the Solar System. We use all available disk-integrated optical data (i.e.,classical dense-in-time photometry obtained from public databases and through alarge collaboration network as well as sparse-in-time individual measurementsfrom a few sky surveys) as an input for the convex inversion method, and derive3D shape models of asteroids, together with their rotation periods andorientations of rotation axes. The key ingredient is the support of more thatone hundred observers who submit their optical data to publicly availabledatabases. We present updated shape models for 36 asteroids, for which massestimates are currently available in the literature or their masses will bemost 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 forthe shape optimization. Moreover, we also present new shape modeldeterminations for 250 asteroids, including 13 Hungarias and 3 near-Earthasteroids.

New and updated convex shape models of asteroids based on optical data from a large collaboration network