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We report on the method developed by Zibetti, Charlot and Rix (2009) toconstruct resolved stellar mass maps of galaxies from optical and NIR imaging.Accurate pixel-by-pixel colour information (specifically g-i and i-H) isconverted into stellar mass-to-light ratios with typical accuracy of 30%, basedon median likelihoods derived from a Monte Carlo library of 50,000 stellarpopulation synthesis models that include dust and updated TP-AGB phaseprescriptions. Hence, surface mass densities are computed. In a pilot study, weanalyze 9 galaxies spanning a broad range of morphologies. Among the mainresults, we find that: i) galaxies appear much smoother in stellar mass mapsthan at any optical or NIR wavelength; ii) total stellar mass estimates basedon unresolved photometry are biased low with respect to the integral ofresolved stellar mass maps, by up to 40%, due to dust obscured regions beingunder-represented in global colours; iii) within a galaxy, on local scalescolours correlate with surface stellar mass density; iv) the slope andtightness of this correlation reflect/depend on the morphology of the galaxy.

Resolved maps of stellar mass and SED of galaxies from optical/NIR imaging and SPS models