  The Euphrosyne asteroid family occupies a unique zone in orbital element
space around 3.15 au and may be an important source of the low-albedo
near-Earth objects. The parent body of this family may have been one of the
planetesimals that delivered water and organic materials onto the growing
terrestrial planets. We aim to characterize the compositional properties as
well as the dynamical properties of the family. We performed a systematic study
to characterize the physical properties of the Euphrosyne family members via
low-resolution spectroscopy using the IRTF telescope. In addition, we performed
smoothed-particle hydrodynamics (SPH) simulations and N-body simulations to
investigate the collisional origin, determine a realistic velocity field, study
the orbital evolution, and constrain the age of the Euphrosyne family. Our
spectroscopy survey shows that the family members exhibit a tight taxonomic
distribution, suggesting a homogeneous composition of the parent body. Our SPH
simulations are consistent with the Euphrosyne family having formed via a
reaccumulation process instead of a cratering event. Finally, our N-body
simulations indicate that the age of the family is 280 Myr +180/-80 Myr, which
is younger than a previous estimate.
