Molecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures

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dc.contributor.authorLaw, Charles J.
dc.contributor.authorLoomis, Ryan A.
dc.contributor.authorTeague, Richard
dc.contributor.authorOberg, Karin, I
dc.contributor.authorCzekala, Ian
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorHuang, Jane
dc.contributor.authorAikawa, Yuri
dc.contributor.authorAlarcon, Felipe
dc.contributor.authorBae, Jaehan
dc.contributor.authorBergin, Edwin A.
dc.contributor.authorBergner, Jennifer B.
dc.contributor.authorBoehler, Yann
dc.contributor.authorBooth, Alice S.
dc.contributor.authorBosman, Arthur D.
dc.contributor.authorCalahan, Jenny K.
dc.contributor.authorCataldi, Gianni
dc.contributor.authorCleeves, L. Ilsedore
dc.contributor.authorFuruya, Kenji
dc.contributor.authorGuzman, Viviana V.
dc.contributor.authorIlee, John D.
dc.contributor.authorLe Gal, Romane
dc.contributor.authorLiu, Yao
dc.contributor.authorLong, Feng
dc.contributor.authorMenard, Francois
dc.contributor.authorNomura, Hideko
dc.contributor.authorQi, Chunhua
dc.contributor.authorSchwarz, Kamber R.
dc.contributor.authorSierra, Anibal
dc.contributor.authorTsukagoshi, Takashi
dc.contributor.authorYamato, Yoshihide
dc.contributor.authorvan't Hoff, Merel L. R.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorWilner, David J.
dc.contributor.authorZhang, Ke
dc.date.accessioned2025-01-20T22:05:48Z
dc.date.available2025-01-20T22:05:48Z
dc.date.issued2021
dc.description.abstractThe Molecules with ALMA at Planet-forming Scales (MAPS) Large Program provides a detailed, high-resolution (similar to 10-20 au) view of molecular line emission in five protoplanetary disks at spatial scales relevant for planet formation. Here we present a systematic analysis of chemical substructures in 18 molecular lines toward the MAPS sources: IM Lup, GM Aur, AS 209, HD 163296, and MWC 480. We identify more than 200 chemical substructures, which are found at nearly all radii where line emission is detected. A wide diversity of radial morphologies-including rings, gaps, and plateaus-is observed both within each disk and across the MAPS sample. This diversity in line emission profiles is also present in the innermost 50 au. Overall, this suggests that planets form in varied chemical environments both across disks and at different radii within the same disk. Interior to 150 au, the majority of chemical substructures across the MAPS disks are spatially coincident with substructures in the millimeter continuum, indicative of physical and chemical links between the disk midplane and warm, elevated molecular emission layers. Some chemical substructures in the inner disk and most chemical substructures exterior to 150 au cannot be directly linked to dust substructure, however, which indicates that there are also other causes of chemical substructures, such as snowlines, gradients in UV photon fluxes, ionization, and radially varying elemental ratios. This implies that chemical substructures could be developed into powerful probes of different disk characteristics, in addition to influencing the environments within which planets assemble. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/ac1434
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/ac1434
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94168
dc.identifier.wosidWOS:000714229800001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal supplement series
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures
dc.typeartículo
dc.volumen257
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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