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HII regions are the birth places of stars, and as such they provide the bestmeasure of current star formation rates (SFRs) in galaxies. The close proximityof the Magellanic Clouds allows us to probe the nature of these star formingregions at small spatial scales. We aim to determine the monochromatic IR bandthat most accurately traces the bolometric IR flux (TIR), which can then beused to estimate an obscured SFR. We present the spatial analysis, viaaperture/annulus photometry, of 16 LMC and 16 SMC HII region complexes usingthe Spitzer IRAC and MIPS bands. UV rocket data and SHASSA H-alpha data arealso included. We find that nearly all of the LMC and SMC HII region SEDs peakaround 70um, from ~10 to ~400 pc from the central sources. As a result, thesizes of HII regions as probed by 70um is approximately equal to the sizes asprobed by TIR (about 70 pc in radius); the radial profile of the 70um flux,normalized by TIR, is constant at all radii (70um ~ 0.45 TIR); the 1-sigmastandard deviation of the 70um fluxes, normalized by TIR, is a lower fractionof the mean (0.05 to 0.12 out to ~220 pc) than the normalized 8, 24, and 160umnormalized fluxes (0.12 to 0.52); and these results are invariant between theLMC and SMC. From these results, we argue that 70um is the most suitable IRband to use as a monochromatic obscured star formation indicator because itmost accurately reproduces the TIR of HII regions in the LMC and SMC and overlarge spatial scales. We also explore the general trends of the 8, 24, 70, and160um bands in the LMC and SMC HII region SEDs, radial surface brightnessprofiles, sizes, and normalized (by TIR) radial flux profiles. We derive anobscured SFR equation that is modified from the literature to use 70umluminosity, SFR(Mo/yr) = 9.7(0.7)x10^{-44} L(70)(ergs/s), which is applicablefrom 10 to 300 pc distance from the center of an HII region.

Spitzer Analysis of HII Region Complexes in the Magellanic Clouds: Determining a Suitable Monochromatic Obscured Star Formation Indicator