  Although low surface brightness galaxies (LSBs) contribute a large fraction
to the number density of galaxies, their properties are still poorly known.
LSBs are often considered dust poor, based only on a few studies. We use, for
the first time, a large sample of LSBs and high surface brightness galaxies
(HSBs) with deep observational data to study their dust properties as a
function of surface brightness. Our sample consists of 1631 optically selected
galaxies at $z < 0.1$ from the North Ecliptic Pole (NEP) wide field. We use the
large set of data available in this field, from UV to FIR. We measured the
optical size and the surface brightness of the targets, and analyzed their
spectral energy distribution using the CIGALE fitting code. We found that the
specific star formation rate and specific infrared luminosity (total infrared
luminosity per stellar mass) remain mostly flat as a function of surface
brightness for both LSBs and HSBs that are star-forming but decline steeply for
the quiescent galaxies. The majority of LSBs in our sample have negligible dust
attenuation (A$_{V} < 0.1$ mag), except for about 4% of them that show
significant attenuation with a mean A$_{V}$ of 0.8 mag. We found that these
LSBs also have a high $\textit{r}$-band mass-to-light ratio ($M/L_r>3$
M$_{\odot}$/L$_{\odot}$), and show similarity to the extreme giant LSBs from
the literature, indicating a possibly higher dust attenuation in giant LSBs as
well. This work provides a large catalog of LSBs and HSBs with detailed
measurements of their several optical and infrared physical properties. Our
results suggest that the dust content of LSBs is more varied than previously
thought, with some of them having significant attenuation making them fainter
than their intrinsic value. This will have serious implications for the
observation and analysis of LSBs with current/upcoming surveys like JWST and
LSST.
