  We estimate the stellar mass for a sample of low surface brightness galaxies
(LSBGs) by fitting their multiband spectral energy distributions (SEDs) to the
stellar population synthesis (SPS) model. The derived stellar masses (log
M*/Msun) span from 7.1 to 11.1, with a mean of log M*/Msun=8.5, which is lower
than that for normal galaxies. The stellar mass-to-light ratio (M/L) in each
band varies little with absolute magnitude, but increases with higher M*. This
trend of M/L with M* is even stronger in bluer bands. In addition, the M/L for
our LSBGs slightly declines from the r band to the longer wavelength bands. The
log M/L_j (j=g,r,i,and z) have relatively tight relations with optical colors
of g-r and g-i. Compared with several representative M/L-color relations
(MLCRs) from literature, our MLCRs based on LSBG data are consistently among
those literature MLCRs previously defined on diverse galaxy samples, and the
existing minor differences between the MLCRs are more caused by the differences
in the SED model ingredients including initial mass function, star formation
history, and stellar population model, and the line fitting techniques, galaxy
samples, and photometric zero-point as well, rather than the galaxy surface
brightness itself which distinguishes LSBGs from HSBGs. Our LSBGs would be very
likely to follow those representative MLCRs previously defined on diverse
galaxy populations, if those main ingredients were taken into account.
