Dust-Induced Systematic Errors in Ultraviolet-Derived Star Formation Rates

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Abstract
Rest-frame far-ultraviolet (FUV) luminosities form the `backbone' of our understanding of star formation at all cosmic epochs. These luminosities are typically corrected for dust by assuming that the tight relationship between the UV spectral slopes and the FUV attenuations of starburst galaxies applies for all star-forming galaxies. Data from seven independent UV experiments demonstrates that quiescent, `normal' star-forming galaxies deviate substantially from the starburst galaxy spectral slope-attenuation correlation, in the sense that normal galaxies are redder than starbursts. Spatially resolved data for the Large Magellanic Cloud suggests that dust geometry and properties, coupled with a small contribution from older stellar populations, cause deviations from the starburst galaxy spectral slope-attenuation correlation. Folding in data for starbursts and ultra-luminous infrared galaxies, it is clear that neither rest-frame UV-optical colors nor UV/H-alpha significantly help in constraining the UV attenuation. These results argue that the estimation of SF rates from rest-frame UV and optical data alone is subject to large (factors of at least a few) systematic uncertainties because of dust, which cannot be reliably corrected for using only UV/optical diagnostics.

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