ALMA 2D super-resolution imaging survey of Ophiuchus Class I/flat spectrum/II disks. II. Statistical analysis of stellar and disk properties

We present a statistical study of stellar and dust disk properties for young stellar objects in the Ophiuchus star-forming region. Building on our previous paper (Shoshi et al. 2025b), which applied two-dimensional super-resolution imaging with PRIISM to ALMA archival Band 6 continuum data and spatially resolved 78 disks, we analyze a sample of 67 systems with robust dust-radius measurements. We combine stellar parameters from the literature, including bolometric temperature $T_{\mathrm{b}\mathrm{o}\mathrm{l}}$, stellar mass $M_{\ast }$, and mass accretion rate ${\dot{M}}_{\mathrm{a}\mathrm{c}\mathrm{c}}$, with disk parameters derived from the super-resolution images, including inclination $i_{\mathrm{d}\mathrm{i}\mathrm{s}\mathrm{k}}$, millimeter luminosity $L_{\mathrm{m}\mathrm{m}}$, and dust radius $R_{95\mathrm{\%}}$. We quantify pairwise correlations and compare their behavior across evolutionary stages (Class I/FS and Class II) and between disks with and without detectable substructures. We identify substructure dependencies in $L_{\mathrm{m}\mathrm{m}}$ and $R_{95\mathrm{\%}}$, indicating that substructures tend to be found preferentially in relatively massive and extended disks. Moreover, we find a tight size-luminosity relation between $R_{95\mathrm{\%}}$ and $L_{\mathrm{m}\mathrm{m}}$. In particular, only Class II disks with substructures exhibit a steeper scaling, $R_{95\mathrm{\%}}\propto L_{\mathrm{m}\mathrm{m}}^{0.8}$, while the other subsamples are broadly consistent with $R_{95\mathrm{\%}}\propto L_{\mathrm{m}\mathrm{m}}^{0.4\text{-}0.5}$. This behavior is qualitatively consistent with disk evolution models in which disks with planet-induced pressure bumps follow a steeper size-luminosity relation than smooth disks. Overall, our results suggest that disk substructures play an important role in shaping the evolution of dust and global disk properties, while providing empirical constraints on accretion, dust trapping, and possible gravitational instability in young disks.