Molecules with ALMA at Planet-forming Scales (MAPS). V. CO Gas Distributions

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dc.contributor.authorZhang, Ke
dc.contributor.authorBooth, Alice S.
dc.contributor.authorLaw, Charles J.
dc.contributor.authorBosman, Arthur D.
dc.contributor.authorSchwarz, Kamber R.
dc.contributor.authorBergin, Edwin A.
dc.contributor.authorOberg, Karin, I
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorGuzman, Viviana V.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorQi, Chunhua
dc.contributor.authorvan 't Hoff, Merel L. R.
dc.contributor.authorLong, Feng
dc.contributor.authorWilner, David J.
dc.contributor.authorHuang, Jane
dc.contributor.authorCzekala, Ian
dc.contributor.authorIlee, John D.
dc.contributor.authorCataldi, Gianni
dc.contributor.authorBergner, Jennifer B.
dc.contributor.authorAikawa, Yuri
dc.contributor.authorTeague, Richard
dc.contributor.authorBae, Jaehan
dc.contributor.authorLoomis, Ryan A.
dc.contributor.authorCalahan, Jenny K.
dc.contributor.authorAlarcon, Felipe
dc.contributor.authorMenard, Francois
dc.contributor.authorLe Gal, Romane
dc.contributor.authorSierra, Anibal
dc.contributor.authorYamato, Yoshihide
dc.contributor.authorNomura, Hideko
dc.contributor.authorTsukagoshi, Takashi
dc.contributor.authorPerez, Laura M.
dc.contributor.authorTrapman, Leon
dc.contributor.authorLiu, Yao
dc.contributor.authorFuruya, Kenji
dc.date.accessioned2025-01-20T22:05:51Z
dc.date.available2025-01-20T22:05:51Z
dc.date.issued2021
dc.description.abstractHere we present high-resolution (15-24 au) observations of CO isotopologue lines from the Molecules with ALMA on Planet-forming Scales (MAPS) ALMA Large Program. Our analysis employs observations of the (J = 2-1) and (1-0) lines of (CO)-C-13 and (CO)-O-18 and the (J = 1-0) line of (CO)-O-17 for five protoplanetary disks. We retrieve CO gas density distributions, using three independent methods: (1) a thermochemical modeling framework based on the CO data, the broadband spectral energy distribution, and the millimeter continuum emission; (2) an empirical temperature distribution based on optically thick CO lines; and (3) a direct fit to the (CO)-O-17 hyperfine lines. Results from these methods generally show excellent agreement. The CO gas column density profiles of the five disks show significant variations in the absolute value and the radial shape. Assuming a gas-to-dust mass ratio of 100, all five disks have a global CO-to-H-2 abundance 10-100 times lower than the interstellar medium ratio. The CO gas distributions between 150 and 400 au match well with models of viscous disks, supporting the long-standing theory. CO gas gaps appear to be correlated with continuum gap locations, but some deep continuum gaps do not have corresponding CO gaps. The relative depths of CO and dust gaps are generally consistent with predictions of planet-disk interactions, but some CO gaps are 5-10 times shallower than predictions based on dust gaps. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/ac1580
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/ac1580
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94171
dc.identifier.wosidWOS:000714237400001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal supplement series
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS). V. CO Gas Distributions
dc.typeartículo
dc.volumen257
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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