ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk

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dc.citation.articleNumberL1en_US
dc.citation.issueNumber1en_US
dc.citation.journalTitleThe Astrophysical Journal Lettersen_US
dc.citation.volumeNumber937en_US
dc.contributor.authorLong, Fengen_US
dc.contributor.authorAndrews, Sean M.en_US
dc.contributor.authorZhang, Shangjiaen_US
dc.contributor.authorQi, Chunhuaen_US
dc.contributor.authorBenisty, Myriamen_US
dc.contributor.authorFacchini, Stefanoen_US
dc.contributor.authorIsella, Andreaen_US
dc.contributor.authorWilner, David J.en_US
dc.contributor.authorBae, Jaehanen_US
dc.contributor.authorHuang, Janeen_US
dc.contributor.authorLoomis, Ryan A.en_US
dc.contributor.authorÖberg, Karin I.en_US
dc.contributor.authorZhu, Zhaohuanen_US
dc.date.accessioned2022-10-28T17:43:00Zen_US
dc.date.available2022-10-28T17:43:00Zen_US
dc.date.issued2022en_US
dc.description.abstractWe present deep high-resolution (∼50 mas, 8 au) Atacama Large Millimeter/submillimeter Array (ALMA) 0.88 and 1.3 mm continuum observations of the LkCa 15 disk. The emission morphology shows an inner cavity and three dust rings at both wavelengths, but with slightly narrower rings at the longer wavelength. Along a faint ring at 42 au, we identify two excess emission features at ∼10σ significance at both wavelengths: one as an unresolved clump and the other as an extended arc, separated by roughly 120° in azimuth. The clump is unlikely to be a circumplanetary disk (CPD) as the emission peak shifts between the two wavelengths even after accounting for orbital motion. Instead, the morphology of the 42 au ring strongly resembles the characteristic horseshoe orbit produced in planet–disk interaction models, where the clump and the arc trace dust accumulation around Lagrangian points L 4 and L 5, respectively. The shape of the 42 au ring, dust trapping in the outer adjacent ring, and the coincidence of the horseshoe ring location with a gap in near-IR scattered light, are all consistent with the scenario of planet sculpting, with the planet likely having a mass between those of Neptune and Saturn. We do not detect pointlike emission associated with a CPD around the putative planet location (0.″27 in projected separation from the central star at a position angle of ∼60°), with upper limits of 70 and 33 μJy at 0.88 and 1.3 mm, respectively, corresponding to dust mass upper limits of 0.02–0.03 M ⊕.en_US
dc.identifier.citationLong, Feng, Andrews, Sean M., Zhang, Shangjia, et al.. "ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk." <i>The Astrophysical Journal Letters,</i> 937, no. 1 (2022) IOP Publishing: https://doi.org/10.3847/2041-8213/ac8b10.en_US
dc.identifier.digitalLong_2022_ApJL_937_L1en_US
dc.identifier.doihttps://doi.org/10.3847/2041-8213/ac8b10en_US
dc.identifier.urihttps://hdl.handle.net/1911/113763en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.titleALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disken_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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