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We present a method to estimate and map the two-dimensional distribution ofdust extinction in the late-type spiral galaxy NGC 959 from the theoretical andobserved flux ratio of optical V and mid-IR (MIR) 3.6 micron images. Our methodis applicable to both young and old stellar populations for a range ofmetallicities, and is not restricted to lines-of-sight toward star-formation(SF) regions. We explore this method using a pixel-based analysis on images ofNGC 959 obtained in the V-band at the Vatican Advanced Technology Telescope(VATT) and at 3.6 micron (L-band) with Spitzer/IRAC. We present the originaland extinction corrected GALEX far-UV (FUV) and near-UV (NUV) images, as wellas optical UBVR images of NGC 959. While the dust lanes are not clearly evidentat GALEX resolution, our dust map clearly traces the dust that can be seensilhouetted against the galaxy's disk in the high-resolution HST images of NGC959. The advantages of our method are: (1) it only depends on two relativelycommon broadband images in the optical V-band and in the MIR at 3.6 micron (butadding a near-UV band improves its fidelity); and (2) it is able to map thetwo-dimensional spatial distribution of dust within a galaxy. This powerfultool could be used to measure the detailed distribution of dust extinctionwithin higher redshift galaxies to be observed with, e.g., the HST/WFC3(optical--near-IR) and JWST (mid-IR), and to distinguish properties of dustwithin galaxy bulges, spiral arms, and inter-arm regions.

Mapping the Spatial Distribution of Dust Extinction in NGC 959 Using Broadband Visible and mid-IR Filters