We investigate whether a correlation exists between the concentration ( c _ { 200 } ) and spin ( \lambda ) parameters of dark matter haloes forming in \Lambda CDM N-body simulations .
In particular , we focus on haloes with virial masses in the range 10 ^ { 11 } \leq M _ { vir } / h ^ { -1 } { M _ { \odot } } \leq 2 \times 10 ^ { 12 } , characteristic of the hosts of Low Surface Brightness ( LSB ) and High Surface Brightness ( HSB ) galaxies .
Our analysis demonstrates that c _ { 200 } and \lambda are anti-correlated .
If we assume that a galaxy disk forms in one of these haloes from baryons that approximately conserved angular momentum during their dissipation into the rotationally supported disk , then it is possible to estimate the disk ’ s central surface density .
For an appropriate choice of mass-to-light ratio , we can place constraints on the central surface brightness of the disk and hence identify the analogues of the host haloes of LSB and HSB galaxies .
We find that our LSB galaxy analogues occupy haloes that have lower concentrations than might be expected based on consideration of the M _ { vir } – c _ { vir } relation for the \Lambda CDM cosmology .
The distribution of concentrations peaks at c _ { 200 } \sim 6 , in good agreement with observational data , although there are important differences between the shapes of the simulated and observationally inferred distributions .
This suggests that LSB galaxies inhabit a biased subsample of the halo population , and that this bias may be an important ingredient for resolving the current debate regarding the structure of LSB galaxy dark matter haloes .