Law, Charles J.Teague, RichardÖberg, Karin I.Rich, Evan A.Andrews, Sean M.Bae, JaehanBenisty, MyriamFacchini, StefanoFlaherty, KevinIsella, AndreaJin, ShengHashimoto, JunHuang, JaneLoomis, Ryan A.Long, FengMuñoz-Romero, Carlos E.Paneque-Carreño, TeresaPérez, Laura M.Qi, ChunhuaSchwarz, Kamber R.Stadler, JochenTsukagoshi, TakashiWilner, David J.Plas, Gerrit van der2023-07-212023-07-212023Law, Charles J., Teague, Richard, Öberg, Karin I., et al.. "Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission." <i>The Astrophysical Journal,</i> 948, (2023) IOP Publishing: https://doi.org/10.3847/1538-4357/acb3c4.https://hdl.handle.net/1911/114975High-spatial-resolution observations of CO isotopologue line emission in protoplanetary disks at mid-inclinations (≈30°–75°) allow us to characterize the gas structure in detail, including radial and vertical substructures, emission surface heights and their dependencies on source characteristics, and disk temperature profiles. By combining observations of a suite of CO isotopologues, we can map the two-dimensional (r, z) disk structure from the disk upper atmosphere, as traced by CO, to near the midplane, as probed by less abundant isotopologues. Here, we present high-angular-resolution (≲0.″1 to ≈0.″2; ≈15–30 au) observations of CO, 13CO, and C18O in either or both J = 2–1 and J = 3–2 lines in the transition disks around DM Tau, Sz 91, LkCa 15, and HD 34282. We derived line emission surfaces in CO for all disks and in 13CO for the DM Tau and LkCa 15 disks. With these observations, we do not resolve the vertical structure of C18O in any disk, which is instead consistent with C18O emission originating from the midplane. Both the J = 2–1 and J = 3–2 lines show similar heights. Using the derived emission surfaces, we computed radial and vertical gas temperature distributions for each disk, including empirical temperature models for the DM Tau and LkCa 15 disks. After combining our sample with literature sources, we find that 13CO line emitting heights are also tentatively linked with source characteristics, e.g., stellar host mass, gas temperature, disk size, and show steeper trends than seen in CO emission surfaces.engExcept where otherwise noted, this work is licensed under a Creative Commons Attribution (CC BY) license.  Permission to reuse, publish, or reproduce the work beyond the terms of the license or beyond the bounds of Fair Use or other exemptions to copyright law must be obtained from the copyright holder.Journal articleLaw_2023_ApJ_948_60https://doi.org/10.3847/1538-4357/acb3c4