  The low metallicities of dwarf irregular galaxies (dIrr) greatly influence
the formation and structure of molecular clouds. These clouds, which consist
primarily of H$_2$, are typically traced by CO, but low metallicity galaxies
are found to have little CO despite ongoing star formation. In order to probe
the conditions necessary for CO core formation in dwarf galaxies, we have used
the catalog of Rubio et al. (2022, in preparation) for CO cores in WLM, a Local
Group dwarf with an oxygen abundance that is 13% of solar. Here we aim to
characterize the galactic environments in which these 57 CO cores formed. We
grouped the cores together based on proximity to each other and strong FUV
emission, examining properties of the star forming region enveloping the cores
and the surrounding environment where the cores formed. We find that high HI
surface density does not necessarily correspond to higher total CO mass, but
regions with higher CO mass have higher HI surface densities. We also find the
cores in star forming regions spanning a wide range of ages show no correlation
between age and CO core mass, suggesting that the small size of the cores is
not due to fragmentation of the clouds with age. The presence of CO cores in a
variety of different local environments, along with the similar properties
between star forming regions with and without CO cores, leads us to conclude
that there are no obvious environmental characteristics that drive the
formation of these CO cores.
