The Palomar Integral Field Spectrograph was used to probe a variety of environments in nine nearby galaxies that span a range of morphological types, luminosities, metallicities, and infrared-to-blue ratios. For the first time, near-infrared spectroscopy was obtained for nuclear or bright HII regions in star-forming galaxies over two spatial dimensions (5.7"x10.0") in the [FeII] (1.257um), [FeII] (1.644um), Paschen beta (1.282um), H2 (2.122um), and Brackett gamma (2.166um) transition lines. These data yield constraints on various characteristics of the star-forming episodes in these regions, including their strength, maturity, spatial variability, and extinction. The HII regions stand out from the nuclei. Unlike observations of nuclear regions, HII region near-infrared observations do not show a spatial coincidence of the line and continuum emission; the continuum and line maps of HII regions usually show distinct and sometimes spatially-separated morphologies. Gauging from Paschen beta and Brackett gamma equivalent widths and luminosities, the HII regions have younger episodes of star formation than the nuclei and more intense radiation fields. Near-infrared line ratio diagnostics suggest that HII regions have "purer" starbursting properties. The correlation between ionizing photon density and mid-infrared color is consistent with the star formation activity level being higher for HII regions than for nuclei. And though the interpretation is complicated, on a purely empirical basis the HII regions show lower Fe1+ abundances than nuclei by an order of magnitude.
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