We present spin-resolved spectroscopy of the accreting white dwarf binary V455 And .
With a suggested spin period of only 67s , it has one of the fastest spinning white dwarfs known .
To study the spectral variability on the spin period of the white dwarf , we observed V455 And with 2 s integration times , which is significantly shorter than the spin rate of the white dwarf .
To achieve this cadence , we used the blue arm of the ISIS spectrograph at the 4.2-m William Herschel Telescope , equipped with an electron multiplying CCD ( EMCCD ) .
Strong coherent signals were detected in our time series , which lead to a robust determination of the spin period of the white dwarf ( P _ { spin } = 67.619 \pm 0.002 s ) .
Folding the spectra on the white dwarf spin period uncovered very complex emission line variations in H \gamma , He I \lambda 4472 and He II \lambda 4686 .
We attribute the observed spin phase dependence of the emission line shape to the presence of magnetically controlled accretion onto the white dwarf via accretion curtains , consistent with an intermediate polar type system .
We are , however , not aware of any specific model that can quantitatively explain the complex velocity variations we detect in our observations .
The orbital variations in the spectral lines indicate that the accretion disc of V455 And is rather structureless , contrary to the disc of the prototype of the intermediate polars , DQ Her .
This work demonstrates the potential of electron multiplying CCDs to observe faint targets at high cadence , as readout noise would make such a study impossible with conventional CCDs .