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We use high spatial resolution maps of stellar mass and infrared flux of theLarge Magellanic Cloud (LMC) to calibrate a conversion between 3.6 and 4.5micron fluxes and stellar mass, M_* = 10^{5.65} * F_{3.6}^{2.85} *F_{4.5}^{-1.85} * (D/0.05)^2 M_solar, where fluxes are in Jy and D is theluminosity distance to the source in Mpc, and to provide an approximateempirical estimate of the fractional internal uncertainty in M_* of0.3*sqrt{N/10^6}, where N is the number of stars in the region. We findevidence that young stars and hot dust contaminate the measurements, butattempts to remove this contamination using data that is far superior than whatis generally available for unresolved galaxies resulted in marginal gains inaccuracy. The scatter among mass estimates for regions in the LMC is comparableto that found by previous investigators when modeling composite populations,and so we conclude that our simple conversion is as precise as possible for thedata and models currently available. Our results allow for a reasonablybottom-heavy initial mass function, such as Salpeter or heavier, and moderatelydisfavor lighter versions such as a diet-Salpeter or Chabrier initial massfunction.

Converting From 3.6 and 4.5 Micron Fluxes to Stellar Mass