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We present new Spitzer 3.6 micron observations of a sample of disk galaxiesspanning over 10 magnitudes in luminosity and ranging in gas fraction from ~10%to over 90%. We use these data to test population synthesis prescriptions forcomputing stellar mass. Many commonly employed models fail to provideself-consistent stellar masses in the sense that the stellar mass estimatedfrom the optical luminosity typically exceeds that estimated from thenear-infrared (NIR) luminosity. This problem is present in models both with andwithout TP-AGB stars, but is more severe in the former. Self-consistency can beachieved if NIR mass-to-light ratios are approximately constant with a meanvalue near 0.5 Msun/Lsun at 3.6 microns. We use the Baryonic Tully-Fisherrelation calibrated by gas rich galaxies to provide an independent estimate ofthe color-mass to light ratio relation. This approach also suggests that thetypical 3.6 micron mass-to-light ratio is 0.5 (0.65 in the K band) forrotationally supported galaxies. These values are consistent with a Kroupa IMF.

The Stellar Masses of Disk Galaxies and the Calibration of Color-Mass to Light Ratio Relations