  Context: Despite the observed signs of large impacts on the surface of Ceres,
there is no confirmed collisional family associated with this dwarf planet.
After a dynamical and photometric study, a sample of 156 asteroids was proposed
as candidate members of a Ceres collisional family.
  Aims: Our main objective is to study the connection between Ceres and a total
of 14 observed asteroids among the candidate's sample to explore their genetic
relationships with Ceres.
  Methods: We obtained visible spectra of these 14 asteroids using the OSIRIS
spectrograph at the 10.4 m Gran Telescopio Canarias(GTC). We computed spectral
slopes in two different wavelength ranges, from 0.49 to 0.80{\mu}m and from
0.80 to 0.92{\mu}m, to compare the values obtained with those on Ceres' surface
previously computed using the Visible and Infrared Spectrometer (VIR)
instrument onboard the NASA Dawn spacecraft. We also calculated the spectral
slopes in the same range for ground-based observations of Cerescollected from
the literature.
  Results: We present the visible spectra and the taxonomy of 14 observed
asteroids. We found that only two of the asteroids are spectrally compatible
with Ceres' surface. Further analysis of those two asteroids indicates that
they are spectrally young and thus less likely to be members of the Ceres
family.
  Conclusions: All in all, our results indicate that most of the 14 observed
asteroids are not likely to belong to a Ceres collisional family. Despite two
of them being spectrally compatible with the young surface of Ceres, further
evaluation is needed to confirm or reject their origin from Ceres.
