Context : Current amount of \sim 500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs , but also of several individual collisional families .

Aims : We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families , among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes .
The remaining models are adopted from the DAMIT database or the literature .

Methods : We revise the preliminary family membership identification by the HCM method according to several additional criteria – taxonomic type , color , albedo , maximum Yarkovsky semi-major axis drift and the consistency with the size-frequency distribution of each family , and consequently we remove interlopers .
We then present the spin-vector distributions for asteroidal families Flora , Koronis , Eos , Eunomia , Phocaea , Themis , Maria and Alauda .
We use a combined orbital- and spin-evolution model to explain the observed spin-vector properties of objects among collisional families .

Results : In general , we observe for studied families similar trends in the ( a _ { \mathrm { p } } , \beta ) space ( proper semi-major axis vs. ecliptic latitude of the spin axis ) : ( i ) larger asteroids are situated in the proximity of the center of the family ; ( ii ) asteroids with \beta > 0 ^ { \circ } are usually found to the right from the family center ; ( iii ) on the other hand , asteroids with \beta < 0 ^ { \circ } to the left from the center ; ( iv ) majority of asteroids have large pole-ecliptic latitudes ( | \beta| \gtrsim 30 ^ { \circ } ) ; and finally ( v ) some families have a statistically significant excess of asteroids with \beta > 0 ^ { \circ } or \beta < 0 ^ { \circ } .
Our numerical simulation of the long-term evolution of a collisional family is capable of reproducing well the observed spin-vector properties .
Using this simulation , we also independently constrain the age of families Flora ( 1.0 \pm 0.5 Gyr ) and Koronis ( 2.5–4 Gyr ) .

Conclusions :