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Variations in the attenuation law have a significant impact on observedspectral energy distributions for galaxies. As one important observationalproperty for galaxies at ultraviolet and infrared wavelength bands, thecorrelation between infrared-to-ultraviolet luminosity ratio and ultravioletcolor index (or ultraviolet spectral slope), i.e., the IRX-UV relation (orIRX-beta relation), offered a widely used recipe for correcting dustattenuation in galaxies, but the usability appears to be in doubt now becauseof considerable dispersion in this relation found by many studies. In thispaper, on the basis of spectral synthesis modeling and spatially resolvedmeasurements of four nearby spiral galaxies, we provide an interpretation ofthe deviation in the IRX-UV relation with variations in the attenuation law.From both theoretical and observational viewpoints, two components in theattenuation curve, the linear background and the 2175 Angstrom bump, aresuggested to be the parameters in addition to the stellar population age(addressed in the first paper of this series) in the IRX-UV function; differentfeatures in the attenuation curve are diagnosed for the galaxies in our sample.Nevertheless, it is often difficult to ascertain the attenuation law forgalaxies in actual observations. Possible reasons for preventing the successfuldetection of the parameters in the attenuation curve are also discussed in thispaper, including the degeneracy of the linear background and the 2175 Angstrombump in observational channels, the requirement for young and dust-rich systemsto study, and the difficulty in accurate estimates of dust attenuations atdifferent wavelength bands.

Characterizing Ultraviolet and Infrared Observational Properties for Galaxies. II. Features of Attenuation Law