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 _ { * } / M _ { \odot } ) span from 7.1 to 11.1 , with a mean of log M _ { * } / M _ { \odot } =8.5 , which is lower than that for normal galaxies .
The stellar mass-to-light ratio ( \gamma ^ { * } ) in each band varies little with the absolute magnitude , but increases with higher M _ { * } .
This trend of \gamma ^ { * } with M _ { * } is even stronger in bluer bands .
In addition , the \gamma ^ { * } for our LSBGs slightly declines from r band to the longer wavelength bands .
The log \gamma _ { * } ^ { j } ( j = g , r , i , and z ) have relatively tight relations with optical colors of g - r and g - i .
Compared with several representative \gamma ^ { * } -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 .