Molecules with ALMA at Planet-forming Scales (MAPS). XIX. Spiral Arms, a Tail, and Diffuse Structures Traced by CO around the GM Aur Disk

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dc.contributor.authorHuang, Jane
dc.contributor.authorBergin, Edwin A.
dc.contributor.authorOberg, Karin, I
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorTeague, Richard
dc.contributor.authorLaw, Charles J.
dc.contributor.authorKalas, Paul
dc.contributor.authorAikawa, Yuri
dc.contributor.authorBae, Jaehan
dc.contributor.authorBergner, Jennifer B.
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.authorCzekala, Ian
dc.contributor.authorIlee, John D.
dc.contributor.authorLe Gal, Romane
dc.contributor.authorGuzman, Viviana V.
dc.contributor.authorLong, Feng
dc.contributor.authorLoomis, Ryan A.
dc.contributor.authorMenard, Francois
dc.contributor.authorNomura, Hideko
dc.contributor.authorQi, Chunhua
dc.contributor.authorSchwarz, Kamber R.
dc.contributor.authorTsukagoshi, Takashi
dc.contributor.authorvan't Hoff, Merel L. R.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorWilner, David J.
dc.contributor.authorYamato, Yoshihide
dc.contributor.authorZhang, Ke
dc.date.accessioned2025-01-20T22:05:38Z
dc.date.available2025-01-20T22:05:38Z
dc.date.issued2021
dc.description.abstractThe concentric gaps and rings commonly observed in protoplanetary disks in millimeter continuum emission have lent the impression that planet formation generally proceeds within orderly, isolated systems. While deep observations of spatially resolved molecular emission have been comparatively limited, they are increasingly suggesting that some disks interact with their surroundings while planet formation is underway. We present an analysis of complex features identified around GM Aur in (CO)-C-12 J = 2 - 1 images at a spatial resolution of similar to 40 au. In addition to a Keplerian disk extending to a radius of similar to 550 au, the CO emission traces flocculent spiral arms out to radii of similar to 1200 au, a tail extending similar to 1800 au southwest of GM Aur, and diffuse structures extending from the north side of the disk up to radii of similar to 1900 au. The diffuse structures coincide with a "dust ribbon" previously identified in scattered light. The large-scale asymmetric gas features present a striking contrast with the mostly axisymmetric, multi-ringed millimeter continuum tracing the pebble disk. We hypothesize that GM Aur's complex gas structures result from late infall of remnant envelope or cloud material onto the disk. The morphological similarities to the SU Aur and AB Aur systems, which are also located in the L1517 cloud, provide additional support to a scenario in which interactions with the environment are playing a role in regulating the distribution and transport of material in all three of these Class II disk systems. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/ac143e
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/ac143e
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94157
dc.identifier.wosidWOS:000714234500001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal supplement series
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS). XIX. Spiral Arms, a Tail, and Diffuse Structures Traced by CO around the GM Aur Disk
dc.typeartículo
dc.volumen257
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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