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How does the low surface brightness galaxies (LSBGs) form stars and assemblethe stellar mass is one of the most important questions to understand the LSBGpopulation. We select a sample of 381 HI bright LSBGs with both Far Ultraviolet(FUV) and Near Infrared (NIR) observation to investigate the star formationrate (SFR) and stellar mass scales, and the growth mode. We measure the UV andNIR radius of our sample, which represent the star-forming and stellar massdistribution scales. We also compare the UV and H band radius-stellar massrelation with the archive data, to identify the SFR and stellar mass structuredifference between the LSBG population and other galaxies. Since galaxy HI masshas a tight correlation with the HI radius, we can also compare the HI and UVradii to understand the distribution of the HI gas and star formationactivities. Our results show that most of the HI selected LSBGs have extendedstar formation structure. The stellar mass distribution of LSBGs may have asimilar structure as the disk galaxies at the same stellar mass bins, while thestar-forming activity of LSBGs happens at a larger radius than the high surfacedensity galaxies, which may help to select the LSBG sample from the wide-fielddeep u band image survey. The HI also distributed at a larger radius, implyinga steeper (or no) Kennicutt-Schmidt relation for LSBGs.

UV and NIR size of the HI selected low surface brightness galaxies