Haumea is one of the most interesting and intriguing transneptunian objects ( TNOs ) .
It is a large , bright , fast rotator , and its spectrum indicates nearly pure water ice on the surface .
It has at least two satellites and a dynamically related family of more than ten TNOs with very similar proper orbital parameters and similar surface properties .
The Haumean family is the only one currently known in the transneptunian belt .
Various models have been proposed but the formation of the family remains poorly understood .
In this work , we have investigated the rotational properties of the family members and unconfirmed family candidates with short-term variability studies , and report the most complete review to date .
We present results based on five years of observations and report the short-term variability of five family members , and seven candidates .
The mean rotational periods , from Maxwellian fits to the frequency distributions , are 6.27 \pm 1.19 h for the confirmed family members , 6.44 \pm 1.16 h for the candidates , and 7.65 \pm 0.54 h for other TNOs ( without relation to the family ) .
According to our study , there is a suggestion that Haumea family members rotate faster than other TNOs , however , the sample of family member is still too limited for a secure conclusion .
We also highlight the fast rotation of 2002 GH _ { 32 } .
This object has a 0.36 \pm 0.02 mag amplitude lightcurve and a rotational period of about 3.98 h. Assuming 2002 GH _ { 32 } is a triaxial object in hydrostatic equilibrium , we derive a lower limit to the density of 2.56 g cm ^ { -3 } .
This density is similar to Haumea ’ s and much more dense than other small TNO densities .