  We present a multiwavelength study of star formation within the nearby M101
Group, including new deep H$\alpha$ imaging of M101 and its two companions. We
perform a statistical analysis of the H$\alpha$ to FUV flux ratios in HII
regions located in three different environments: M101's inner disk, M101's
outer disk, and M101's lower mass companion galaxy NGC~5474. We find that, once
bulk radial trends in extinction are taken into account, both the median and
scatter in F$_{\rm H\alpha}/$F$_{\rm FUV}$ in HII regions are invariant across
all of these environments. Also, using Starburst99 models, we are able to
qualitatively reproduce the distributions of F$_{\rm H\alpha}/$F$_{\rm FUV}$
throughout these different environments using a standard Kroupa IMF, hence we
find no need to invoke truncations in the upper mass end of the IMF to explain
the young star-forming regions in the M101 Group even at extremely low surface
density. This implies that star formation in low density environments differs
from star formation in high density environments only by intensity and not by
cloud-to-cloud physics.
