with the spin properties of their surrounding dark matter [haloes]{} [@fall_1980]. The simplest model explains this correlation via angular momentum conservation and assuming baryons and dark matter initially share the same specific angular momentum distribution [@mestel_1963]. Even though subsequent models paint a more complex picture, this link continues to exist [e.g. @dalcanton_1997; @mo_1998; @navarro_2000; @abadi_2003; @bett_2010]. Consequently, the halo spin is an important parameter in many semi-analytic models of galaxy formation [@kauffmann_1993; @kauffmann_1997; @frenk_1997; @cole_2000; @benson_2001; @bower_2006; @croton_2006; @delucia_2007; @bertone_2007; @font_2008; @benson_2012] and a number of studies have investigated the spin of individual dark matter [haloes]{} in cosmological simulations [@peebles_1969; @bullock_2001; @hetznecker_2006; @bett_2007; @maccio_2007; @gottlober_2007; @knebe_2008; @antonuccio_2010; @wang_2011b; @lacerna_2012; @trowland_2012; @bryan_2013].

Due to a lack of resolution in previous generations of large cosmological simulations, subhalo spins have not been thoroughly investigated so far, despite their application within current semi-analytic models [@guo_2011]. Initial work by @lee_2013 analyzed the spins of the two most massive substructures of Local Group like systems in the Millennium-II simulation [@boylan_kolchin_2009] and revealed possible consequences for the application of subhalo spins to near-field cosmology.

@onions_2013 investigated the spin distribution of sub[haloes]{}in two high resolution simulations of a Milky Way-like halo (the Aquarius simulation [@springel_aquarius_2008] and the [<span 