  We quantify the spatial distributions of dense cores in three spatially
distinct areas of the Orion B star-forming region. For L1622, NGC2068/NGC2071
and NGC2023/NGC2024 we measure the amount of spatial substructure using the
$\mathcal{Q}$-parameter and find all three regions to be spatially
substructured ($\mathcal{Q} < 0.8$). We quantify the amount of mass segregation
using $\Lambda_{\rm MSR}$ and find that the most massive cores are mildly mass
segregated in NGC2068/NGC2071 ($\Lambda_{\rm MSR} \sim 2$), and very mass
segregated in NGC2023/NGC2024 ($\Lambda_{\rm MSR} = 28^{+13}_{-10}$ for the
four most massive cores). Whereas the most massive cores in L1622 are not in
areas of relatively high surface density, or deeper gravitational potentials,
the massive cores in NGC2068/NGC2071 and NGC2023/NGC2024 are significantly so.
Given the low density (10 cores pc$^{-2}$) and spatial substructure of cores in
Orion B, the mass segregation cannot be dynamical. Our results are also
inconsistent with simulations in which the most massive stars form via
competitive accretion, and instead hint that magnetic fields may be important
in influencing the primordial spatial distributions of gas and stars in
star-forming regions.
