The stellar mass - physical effective radius relation for dwarf galaxies
  in low-density environments
  The scaling relation between stellar mass ($M_{*}$) and physical effective
radius ($r_{e}$) has been well-studied using wide spectroscopic surveys.
However, these surveys suffer from severe surface brightness incompleteness in
the dwarf galaxy regime, where the relation is poorly constrained. In this
study, I use a Bayesian empirical model to constrain the power-law exponent
$\beta$ of the $M_{*}$-$r_{e}$ relation for late-type dwarfs
($10^{7}$$\leq$$M_{*}$/$M_{\odot}$$\leq$$10^{9}$) using a sample of 188
isolated low surface brightness (LSB) galaxies, accounting for observational
incompleteness. Surprisingly, the best-fitting model ($\beta$=0.40$\pm$0.07)
indicates that the relation is significantly steeper than would be expected
from extrapolating canonical models into the dwarf galaxy regime. Nevertheless,
the best fitting $M_{*}$-$r_{e}$ relation closely follows the distribution of
known dwarf galaxies. These results indicate that extrapolated canonical models
over-predict the number of large dwarf (i.e. LSB) galaxies, including
ultra-diffuse galaxies (UDGs), explaining why they are over-produced by some
semi-analytic models. The best-fitting model also constrains the power-law
exponent of the physical size distribution of UDGs to
$n\mathrm{[dex^{-1}]}\propto$$~r_{e}^{3.54\pm0.33}$, consistent to within
1$\sigma$ of the corresponding value in cluster environments and with the
theoretical scenario in which UDGs occupy the high-spin tail of the normal
dwarf galaxy population.
