Galaxy disc central surface brightness distribution in the optical and near-infrared bands

To study the disc central surface brightness($\mu_0$) distribution in optical and near-infrared bands, we select 708 disc-dominated galaxies within a fixed distance of 57 Mpc from SDSS DR7 and UKIDSS DR10. Then we fit $\mu_0$ distribution by using single and double Gaussianprofiles with an optimal bin size for the final sample of 538 galaxies in optical $griz$ bands and near-infrared $YJHK$ bands. Among the 8 bands, we find that $\mu_{0}$ distribution in optical bands can not be much better fitted with double Gaussianprofiles. However, for all the near-infrared bands, the evidence of being better fitted by using double Gaussianprofiles is positive. Especially for $ K$ band, the evidence of a double Gaussianprofile being better than a single Gaussianprofile for $\mu_{0}$ distribution is very strong, the reliability of which can be approved by 1000 times test for our sample. No dust extinction correction is applied. The difference of $\mu_{0}$ distribution between optical and near-infrared bands could be caused by the effect of dust extinction in optical bands. Due to the sample selection criteria, our sample is not absolutely complete. However, the sample incompleteness does not change the double Gaussiandistribution of $\mu_{0}$ in $ K$ band. Furthermore, we discuss some possible reasons for the fitting results of $\mu_{0}$ distribution in $ K$ band. Conclusively, the double Gaussiandistribution of $\mu_{0}$ in $ K$ bandfor our sample may depend on bulge-to-disk ratio, color and disk scalelength, rather than the inclination of sample galaxies, bin size and statistical fluctuations.