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Spectro-photometry of debris disks in total intensity and polarimetry canprovide new insight into the properties of the dust grains therein (sizedistribution and optical properties).  We aim to constrain the morphology of the highly inclined debris disk HD32297. We also intend to obtain spectroscopic and polarimetric measurements toretrieve information on the particle size distribution within the disk forcertain grain compositions.  We observed HD 32297 with SPHERE in Y, J, and H bands in total intensity andin J band in polarimetry. The observations are compared to synthetic models ofdebris disks and we developed methods to extract the photometry in totalintensity overcoming the data-reduction artifacts, namely the self-subtraction.The spectro-photometric measurements averaged along the disk mid-plane are thencompared to model spectra of various grain compositions.  These new images reveal the very inner part of the system as close as 0.15".The disk image is mostly dominated by the forward scattering making one side(half-ellipse) of the disk more visible, but observations in total intensityare deep enough to also detect the back side for the very first time. Theimages as well as the surface brightness profiles of the disk rule out thepresence of a gap as previously proposed. We do not detect any significantasymmetry between the northeast and southwest sides of the disk. The spectralreflectance features a "gray to blue" color which is interpreted as thepresence of grains far below the blowout size.  The presence of sub-micron grains in the disk is suspected to be the resultof gas drag and/or "avalanche mechanisms". The blue color of the disk could befurther investigated with additional total intensity and polarimetricobservations in K and H bands respectively to confirm the spectral slope andthe fraction of polarization.

Spatially resolved spectroscopy of the debris disk HD 32297: Further evidence of small dust grains