Molecules with ALMA at Planet-forming Scales (MAPS). IX. Distribution and Properties of the Large Organic Molecules HC<sub>3</sub>N, CH<sub>3</sub>CN, and <i>c</i>-C<sub>3</sub>H<sub>2</sub>

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dc.contributor.authorIlee, John D.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorBooth, Alice S.
dc.contributor.authorAikawa, Yuri
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorBae, Jaehan
dc.contributor.authorBergin, Edwin A.
dc.contributor.authorBergner, Jennifer B.
dc.contributor.authorBosman, Arthur D.
dc.contributor.authorCataldi, Gianni
dc.contributor.authorCleeves, L. Ilsedore
dc.contributor.authorCzekala, Ian
dc.contributor.authorGuzman, Viviana V.
dc.contributor.authorHuang, Jane
dc.contributor.authorLaw, Charles J.
dc.contributor.authorLe Gal, Romane
dc.contributor.authorLoomis, Ryan A.
dc.contributor.authorMenard, Francois
dc.contributor.authorNomura, Hideko
dc.contributor.authorOberg, Karin, I
dc.contributor.authorQi, Chunhua
dc.contributor.authorSchwarz, Kamber R.
dc.contributor.authorTeague, Richard
dc.contributor.authorTsukagoshi, Takashi
dc.contributor.authorWilner, David J.
dc.contributor.authorYamato, Yoshihide
dc.contributor.authorZhang, Ke
dc.date.accessioned2025-01-20T22:05:35Z
dc.date.available2025-01-20T22:05:35Z
dc.date.issued2021
dc.description.abstractThe precursors to larger, biologically relevant molecules are detected throughout interstellar space, but determining the presence and properties of these molecules during planet formation requires observations of protoplanetary disks at high angular resolution and sensitivity. Here, we present 0.'' 3 observations of HC3N, CH3CN, and c-C3H2 in five protoplanetary disks observed as part of the Molecules with ALMA at Planet-forming Scales (MAPS) Large Program. We robustly detect all molecules in four of the disks (GM Aur, AS 209, HD 163296, and MWC 480) with tentative detections of c-C3H2 and CH3CN in IM Lup. We observe a range of morphologies-central peaks, single or double rings-with no clear correlation in morphology between molecule or disk. Emission is generally compact and on scales comparable with the millimeter dust continuum. We perform both disk-integrated and radially resolved rotational diagram analysis to derive column densities and rotational temperatures. The latter reveals 5-10 times more column density in the inner 50-100 au of the disks when compared with the disk-integrated analysis. We demonstrate that CH3CN originates from lower relative heights in the disks when compared with HC3N, in some cases directly tracing the disk midplane. Finally, we find good agreement between the ratio of small to large nitriles in the outer disks and comets. Our results indicate that the protoplanetary disks studied here are host to significant reservoirs of large organic molecules, and that this planet- and comet-building material can be chemically similar to that in our own solar system. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/ac1441
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/ac1441
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94153
dc.identifier.wosidWOS:000714243800001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal supplement series
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS). IX. Distribution and Properties of the Large Organic Molecules HC<sub>3</sub>N, CH<sub>3</sub>CN, and <i>c</i>-C<sub>3</sub>H<sub>2</sub>
dc.typeartículo
dc.volumen257
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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