$R_{\rm e}$. II. Understanding the IC 3475 galaxy type, including ultra-diffuse galaxy, structural scaling relations

It is explained why relatively gas-poor ultra-diffuse galaxies (UDGs), a subset of IC 3475 galaxy types, do not have unexpectedly large sizes but large sizes that are in line with expectations from the curved size-luminosity relation defined by brighter early-type galaxies (ETGs). These UDGs extend the faint end of the (absolute magnitude, $\mathfrak{M}$)-log(S\'ersic index, $n$) and $\mathfrak{M}$-(central surface brightness, $\mu_{\rm 0}$) relations defined by all ETGs, leading to the large effective half-light radii, $R_{\rm e}$, in these UDGs. It is detailed how the scatter in $\mu_{\rm 0}$, at a given $\mathfrak{M}$, relates to variations in the galaxies' values of $n$ and effective surface brightness, $\mu_{\rm e}$. These variations map into changes in $R_{\rm e}$ and produce the scatter about the $\mathfrak{M}$-$R_{\rm e}$ relation at fixed $\mathfrak{M}$. Similarly, the scatter in $\mathfrak{M}$, at fixed $\mu_{\rm 0}$ and $n$, can be mapped into changes in $R_{\rm e}$. The suggestion that there may be two types of relatively gas-poor UDGs appears ill-founded, arising from the scatter about the $\mathfrak{M}$-$\mu_{\rm 0}$ relation. The increased scatter about the faint end of the $\mathfrak{M}$-$R_{\rm e}$ relation and the smaller scatter about $\mathfrak{M}$-(isophotal radii, $R_{\rm iso}$) relations are explained. Artificial and potentially misleading size-luminosity relations for UDGs are also addressed. Finally, expected trends with dynamical mass, and evolutionary pathways towards relatively gas-rich galaxies, are briefly discussed. Hopefully, the understanding presented here will prove helpful for interpreting the many low surface brightness galaxies that the Large Synoptic Survey Telescope will detect.