Spectral energy distribution (SED) fitting of stellar population synthesis models is an important and popular way to constrain the physical parameters—e.g., the ages, metallicities, masses for stellar population analysis. The previous works suggest that both blue-bands and red-bands photometry works for the SED-fitting. Either blue-domained or red-domained SED-fitting usually lead to the unreliable or biased results. Meanwhile, it seems that extending the wavelength coverage could be helpful. Since the Galaxy Evolution Explorer (GALEX) and Wide-field Infrared Survey Explorer (WISE) provide the FUV/NUV and mid-infrared W1/W2\documentclass[12pt]{minimal}
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\begin{document}$W1/W2$\end{document} band data, we extend the SED-fitting to a wider wavelength coverage. In our work, we analyzed the effect of adding the FUV/NUV and W1/W2\documentclass[12pt]{minimal}
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\begin{document}$W1/W2$\end{document} band to the optical and near-infrared UBVRIJHK\documentclass[12pt]{minimal}
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\begin{document}$\mathit{UBVRIJHK}$\end{document} bands for the fitting with the (Bruzual and Charlot in Mon. Not. R. Astron. Soc. 344, 1000, 2003) (BC03) models and galev models. It is found that the FUV/NUV bands data affect the fitting results of both ages and metallicities much more significantly than that of the WISE W1/W2\documentclass[12pt]{minimal}
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\begin{document}$W1/W2$\end{document} band with the BC03 models. While for the galev models, the effect of the WISE W1/W2\documentclass[12pt]{minimal}
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\begin{document}$W1/W2$\end{document} band for the metallicity fitting seems comparable to that of GALEX FUV/NUV bands, but for age the effect of the W1/W2\documentclass[12pt]{minimal}
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\begin{document}$W1/W2$\end{document} band seems less crucial than that of the FUV/NUV bands. Thus we conclude that the 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 photometry precision) are required.
