Context : The transneptunian region of the solar system is populated by a wide variety of icy bodies showing great diversity in orbital behavior , size , surface color , and composition .

Aims : The dwarf planet ( 136108 ) Haumea is among the largest transneptunian objects and is a very fast rotator ( \sim 3.9h ) .
This dwarf planet displays a highly elongated shape and hosts two small moons that are covered with crystalline water ice , similar to their central body .
A particular region of interest is the Dark Red Spot ( DRS ) identified on the surface of Haumea from multiband light-curve analysis ( Lacerda et al .
2008 ) .
Haumea is also known to be the largest member of the sole TransNeptunian Objects ( TNO ) family known to date , and an outcome of a catastrophic collision that is likely responsible for the unique characteristics of Haumea .

Methods : We report here on the analysis of a new set of near-infrared Laser Guide Star assisted observations of Haumea obtained with the Integral Field Unit ( IFU ) Spectrograph for INtegral Field Observations in the Near Infrared ( SINFONI ) at the European Southern Observatory ( ESO ) Very Large Telescope ( VLT ) Observatory .
Combined with previous data published by Dumas et al .
( 2011 ) , and using light-curve measurements in the optical and far infrared to associate each spectrum with its corresponding rotational phase , we were able to carry out a rotationally resolved spectroscopic study of the surface of Haumea .

Results : We describe the physical characteristics of the crystalline water ice present on the surface of Haumea for both regions , in and out of the DRS , and analyze the differences obtained for each individual spectrum .
The presence of crystalline water ice is confirmed over more than half of the surface of Haumea .
Our measurements of the average spectral slope ( 1.45 \pm 0.82 % by 100 nm ) confirm the redder characteristic of the spot region .
Detailed analysis of the crystalline water-ice absorption bands do not show significant differences between the DRS and the remaining part of the surface .
We also present the results of applying Hapke modeling to our data set .
The best spectral fit is obtained with a mixture of crystalline water ice ( grain sizes smaller than 60 \mu m ) with a few percent of amorphous carbon .
Improvements to the fit are obtained by adding \sim 10 % of amorphous water ice .
Additionally , we used the IFU-reconstructed images to measure the relative astrometric position of the largest satellite Hi ‘ iaka and determine its orbital elements .
An orbital solution was computed with our genetic-based algorithm GENOID and our results are in full agreement with recent results .

Conclusions :