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IC342 is a nearby, late-type spiral galaxy with a young nuclear star clustersurrounded by several giant molecular clouds. The IC342 nuclear region issimilar to the Milky Way and therefore provides an interesting comparison. Weexplore star formation in the nucleus using radio recombination line (RRL) andcontinuum emission at 5, 6.7, 33, and 35 GHz with the JVLA. These radio tracersare largely unaffected by dust and therefore sensitive to all of the thermalemission from the ionized gas produced by early-type stars. We resolve twocomponents in the RRL and continuum emission within the nuclear region that lieeast and west of the central star cluster. These components are associated bothspatially and kinematically with two giant molecular clouds. We model theseregions in two ways: a simple model consisting of uniform gas radiating inspontaneous emission, or as a collection of many compact HII regions innon-LTE. The multiple HII region model provides a better fit to the data andpredicts many dense (ne ~ 10^4-10^5 cm-3), compact (< 0.1 pc) HII regions. Forthe whole nuclear region as defined by RRL emission, we estimate a hydrogenionizing rate of NL ~ 2 x 10^{52} s^{-1}, corresponding to equivalent ~ 2000 O6stars and a star formation rate of ~ 0.15 Msun/year. We detect radio continuumemission west of the southern molecular mini spiral arm, consistent withtrailing spiral arms.

JVLA Observations of IC342: Probing Star Formation in the Nucleus