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We develop a novel approach to measure dust attenuation properties ofgalaxies, including the dust opacity, shape of the attenuation curve and thestrength of the 2175{\AA} absorption feature. From an observed spectrum, themethod uses a model-independent approach to derive a relative attenuationcurve, with absolute amplitude calibrated using NIR photometry. Thedust-corrected spectrum is fitted with stellar population models to derive thedust-free model spectrum, which is compared with the observed SED/spectrum fromNUV to NIR to determine dust attenuation properties. We apply this method toinvestigate dust attenuation on kpc scales, using a sample of 134 galaxies withintegral field spectroscopy from MaNGA, NIR imaging from 2MASS, and NUV imagingfrom Swift/UVOT. We find the attenuation curve slope and the 2175{\AA} bump inboth optical and NUV span a wide range at kpc scales. The slope is shallower athigher optical opacity, regardless of the specific star formation rate (sSFR),minor-to-major axis ratio (b/a) of galaxies and the location of spaxels withinindividual galaxies. The 2175{\AA} bump presents a strong negative correlationwith the sSFR, while the correlations with the optical opacity, b/a and thelocation within individual galaxies are all weak. All these trends appear to beindependent of the stellar mass of galaxies. Our results support the scenariothat the variation of the 2175{\AA} bump is driven predominantly by processesrelated to star formation, such as the destruction of small dust grains by UVradiation in star-forming regions.

Mapping dust attenuation and the 2175 {\AA} bump at kpc scales in nearby galaxies