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We present robust statistical estimates of the accuracy of early-type galaxystellar masses derived from spectral energy distribution (SED) fitting asfunctions of various empirical and theoretical assumptions. Using large samplesconsisting of 40,000 galaxies from the Sloan Digital Sky Survey, of which 5,000are also in the UKIRT Infrared Deep Sky Survey, with spectroscopic redshifts inthe range 0.05 \leq z \leq 0.095, we test the reliability of some commonly usedstellar population models and extinction laws for computing stellar masses.Spectroscopic ages (t), metallicities (Z), and extinctions (A) are alsocomputed from fits to SDSS spectra using various population models. Theseconstraints are used in additional tests to estimate the systematic errors inthe stellar masses derived from SED fitting, where t, Z, and A are typicallyleft as free parameters. We find reasonable agreement in mass estimates amongstellar population models, with variation of the IMF and extinction lawyielding systematic biases on the mass of nearly a factor of 2, in agreementwith other studies. Removing the near-infrared bands changes the statisticalbias in mass by only 0.06 dex, adding uncertainties of 0.1 dex at the 95% CL.In contrast, we find that removing an ultraviolet band is more critical,introducing 2{\sigma} uncertainties of 0.15 dex. Finally, we find that stellarmasses are less affected by absence of metallicity and/or dust extinctionknowledge. However, there is a definite systematic offset in the mass estimatewhen the stellar population age is unknown, up to a factor of 2.5 for very old(12 Gyr) stellar populations. We present the stellar masses for our sample,corrected for the measured systematic biases due to photometrically determinedages, finding that age errors produce lower stellar masses by 0.15 dex, witherrors of 0.02 dex at the 95% CL for the median stellar age subsample.

SPIDER - V. Measuring Systematic Effects in Early-Type Galaxy Stellar Masses from Photometric SED Fitting