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Spectral energy distribution (SED) fitting of stellar population synthesismodels is an important and popular way to constrain the physical parameters---e.g., the ages, metallicities, masses for stellar population analysis. Theprevious works suggest that both blue-bands and red-bands photometry works forthe SED-fitting. Either blue-domained or red-domained SED-fitting usually leadto the unreliable or biased results. Meanwhile, it seems that extending thewavelength coverage could be helpful. Since the Galaxy Evolution Explorer ({\itGALEX}) and Wide-field Infrared Survey Explorer (WISE) provide the FUV/NUV andmid-infrared $W1$/$W2$ band data, we extend the SED-fitting to a widerwavelength coverage. In our work, we analyzed the effect of adding the FUV/NUVand $W1$/$W2$ band to the optical and near-infrared $UBVRIJHK$ bands for thefitting with the Bruzual \& Charlot 2003 (BC03) models and {\sc galev} models.It is found that the FUV/NUV bands data affect the fitting results of both agesand metallicities much more significantly than that of the WISE $W1$/$W2$ bandwith the BC03 models. While for the {\sc galev} models, the effect of the WISE$W1$/$W2$ band for the metallicity fitting seems comparable to that of {\itGALEX} FUV/NUV bands, but for age the effect of the $W1$/$W2$ band seems lesscrucial than that of the FUV/NUV bands. Thus we conclude that the {\it GALEX}FUV/NUV bands are more crucial for the SED-fitting of ages and metallicities,than the other bands, and the high-quality UV data (with high photometryprecision) are required.

The Effects of the WISE/GALEX Photometry for the SED-Fitting with M31 Star Clusters and Candidates