dust extinction ($A_V$=0.1-1.6) for our sample galaxies. The left panel shows the SED fitting for one example of LSBGs (same as in Fig. \[Fig2\], but the derived age is 2.10 Gyr), the middle panel shows the SED fitting for one example of HSBGs (same as in Fig. \[Fig2\] but the derived age is 1.96 Gyr), and the right panel shows the histogram distributions of the derived ages of LSBGs (shade region) and HSBGs (dashed-line) with bin of 0.2 Gyr. []{data-label="Fig3"}](ms471fig3a.eps "fig:"){width="4.8cm" height="4.8cm"} ![The fitting results with PEGASE model and varying dust extinction ($A_V$=0.1-1.6) for our sample galaxies. The left panel shows the SED fitting for one example of LSBGs (same as in Fig. \[Fig2\], but the derived age is 2.10 Gyr), the middle panel shows the SED fitting for one example of HSBGs (same as in Fig. \[Fig2\] but the derived age is 1.96 Gyr), and the right panel shows the histogram distributions of the derived ages of LSBGs (shade region) and HSBGs (dashed-line) with bin of 0.2 Gyr. []{data-label="Fig3"}](ms471fig3b.eps "fig:"){width="4.8cm" height="4.8cm"} ![The fitting results with PEGASE model and varying dust extinction ($A_V$=0.1-1.6) for our sample galaxies. The left panel shows the SED fitting for one example of LSBGs (same 