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We study dust attenuation curves of 230,000 individual galaxies in the localuniverse, ranging from quiescent to intensely star-forming systems, usingGALEX, SDSS, and WISE photometry calibrated on Herschel-ATLAS. We use a newmethod of constraining SED fits with infrared luminosity (SED+LIR fitting), andparameterized attenuation curves determined with the CIGALE SED fitting code.Attenuation curve slopes and UV bump strengths are reasonably well constrainedindependently from one another. We find that $A_{\lambda}/A_V$ attenuationcurves exhibit a very wide range of slopes that are on average as steep as theSMC curve slope. The slope is a strong function of optical opacity. Opaquegalaxies have shallower curves - in agreement with recent radiate transfermodels. The dependence of slopes on the opacity produces an apparent dependenceon stellar mass: more massive galaxies having shallower slopes. Attenuationcurves exhibit a wide range of UV bump amplitudes, from none to MW-like; withan average strength 1/3 of the MW bump. Notably, local analogs of high-redshiftgalaxies have an average curve that is somewhat steeper than the SMC curve,with a modest UV bump that can be to first order ignored, as its effect on thenear-UV magnitude is 0.1 mag. Neither the slopes nor the strengths of the UVbump depend on gas-phase metallicity. Functional forms for attenuation laws arepresented for normal star-forming galaxies, high-z analogs and quiescentgalaxies. We release the catalog of associated SFRs and stellar masses(GSWLC-2).

Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs