will be given in Sect.4.

![Histogram distributions of $\mu_{0}$(B) (with bin of 0.1) and redshift (with bin of 0.01) for our sample galaxies with FUV-to-NIR multiwavelength observations. The shaded regions refer to the LSBGs with $\mu_{0}$(B) $\geq$ 22 mag arcsec$^{-2}$, and the dashed-lines refer to the HSBGs. []{data-label="his.mu.z"}](ms471fig1a.eps "fig:"){width="5.5cm" height="5.5cm"} ![Histogram distributions of $\mu_{0}$(B) (with bin of 0.1) and redshift (with bin of 0.01) for our sample galaxies with FUV-to-NIR multiwavelength observations. The shaded regions refer to the LSBGs with $\mu_{0}$(B) $\geq$ 22 mag arcsec$^{-2}$, and the dashed-lines refer to the HSBGs. []{data-label="his.mu.z"}](ms471fig1b.eps "fig:"){width="5.5cm" height="5.5cm"}

Evolutionary Synthesis Model PEGASE {#sect:data}
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Evolutionary population synthesis is a powerful tool of interpretation of the integrated spectrophotometric observations of galaxies. The most common method of model-observation comparison for stellar population analysis in galaxies or star clusters is SED fitting, with either least-squares or chi-squared minimization technique (Kong et al. 2000; Gavazzi et al. 2002; Jiang et al. 2003; Li et al. 2004a,b; Fan et al. 2006; Ma et al. 2002a,b, 2007, 2009a,b; Wang et al. 2010). There are several EPS models popularly used in astrophysical studies (Chen et al. 2009, 2010 for references therein). We use PEGASE in this work.

PEGASE is an 