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We present the results of a study of the late-type spiral galaxy NGC 0959,before and after application of the pixel-based dust extinction correctiondescribed in Tamura et al. 2009 (Paper I). Galaxy Evolution Explorer (GALEX)far-UV (FUV) and near-UV (NUV), ground-based Vatican Advanced TechnologyTelescope (VATT) UBVR, and Spitzer/Infrared Array Camera (IRAC) 3.6, 4.5, 5.8,and 8.0 micron images are studied through pixel Color-Magnitude Diagrams(pCMDs) and pixel Color-Color Diagrams (pCCDs). We define groups of pixelsbased on their distribution in a pCCD of (B - 3.6 micron) versus (FUV - U)colors after extinction correction. In the same pCCD, we trace their locationsbefore the extinction correction was applied. This shows that selecting pixelgroups is not meaningful when using colors uncorrected for dust. We also tracethe distribution of the pixel groups on a pixel coordinate map of the galaxy.We find that the pixel-based (two-dimensional) extinction correction is crucialto reveal the spatial variations in the dominant stellar population, averagedover each resolution element. Different types and mixtures of stellarpopulations, and galaxy structures such as a previously unrecognized bar,become readily discernible in the extinction-corrected pCCD and as coherentspatial structures in the pixel coordinate map.

Lifting the Veil of Dust from NGC 0959: The Importance of a Pixel-Based 2D Extinction Correction