UV and NIR size of the HI selected low surface brightness galaxies
  How does the low surface brightness galaxies (LSBGs) form stars and assemble
the stellar mass is one of the most important questions to understand the LSBG
population. We select a sample of 381 HI bright LSBGs with both Far Ultraviolet
(FUV) and Near Infrared (NIR) observation to investigate the star formation
rate (SFR) and stellar mass scales, and the growth mode. We measure the UV and
NIR radius of our sample, which represent the star-forming and stellar mass
distribution scales. We also compare the UV and H band radius-stellar mass
relation with the archive data, to identify the SFR and stellar mass structure
difference between the LSBG population and other galaxies. Since galaxy HI mass
has a tight correlation with the HI radius, we can also compare the HI and UV
radii to understand the distribution of the HI gas and star formation
activities. Our results show that most of the HI selected LSBGs have extended
star formation structure. The stellar mass distribution of LSBGs may have a
similar structure as the disk galaxies at the same stellar mass bins, while the
star-forming activity of LSBGs happens at a larger radius than the high surface
density galaxies, which may help to select the LSBG sample from the wide-field
deep u band image survey. The HI also distributed at a larger radius, implying
a steeper (or no) Kennicutt-Schmidt relation for LSBGs.
