Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission

High spatial resolution observations of CO isotopologue line emission in protoplanetary disks at mid-inclinations (${\approx}$30-75{\deg}) allow us to characterize the gas structure detail, including radial and vertical substructures, surface heights their dependencies on source characteristics, disk temperature profiles. By combining a suite isotopologues, we can map 2D (r, z) from upper atmosphere, as traced by CO, near midplane, probed less abundant isotopologues. Here, present high angular (${\lesssim}$0."1 ${\approx}$0."2; ${\approx}$15-30 au) $^{13}$CO, C$^{18}$O either or both J=2-1 J=3-2 lines transition around DM Tau, Sz 91, LkCa 15, HD 34282. We derived surfaces for all $^{13}$CO Tau 15 disks. With these observations, do not resolve any disk, which is instead consistent with originating midplane. Both show similar heights. Using surfaces, computed distributions each empirical models After our sample literature sources, find that emitting are also tentatively linked e.g., stellar host mass, temperature, size, steeper trends than seen surfaces.