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dc.contributor.authorHendler, Nathanial P
dc.contributor.authorPinilla, Paola
dc.contributor.authorPascucci, Ilaria
dc.contributor.authorPohl, Adriana
dc.contributor.authorMulders, Gijs
dc.contributor.authorHenning, Thomas
dc.contributor.authorDong, Ruobing
dc.contributor.authorClarke, Cathie
dc.contributor.authorOwen, James
dc.contributor.authorHollenbach, David
dc.date.accessioned2018-11-16T23:00:14Z
dc.date.available2018-11-16T23:00:14Z
dc.date.issued2018-03
dc.identifier.citationNathanial P Hendler, Paola Pinilla, Ilaria Pascucci, Adriana Pohl, Gijs Mulders, Thomas Henning, Ruobing Dong, Cathie Clarke, James Owen, David Hollenbach; A likely planet-induced gap in the disc around T Cha, Monthly Notices of the Royal Astronomical Society: Letters, Volume 475, Issue 1, 21 March 2018, Pages L62–L66, https://doi.org/10.1093/mnrasl/slx184en_US
dc.identifier.issn1745-3925
dc.identifier.issn1745-3933
dc.identifier.doi10.1093/mnrasl/slx184
dc.identifier.urihttp://hdl.handle.net/10150/631023
dc.description.abstractWe present high-resolution (0.11 x 0.06 arcsec(2)) 3mm ALMA observations of the highly inclined transition disc around the star T Cha. Our continuum image reveals multiple dust structures: an inner disc, a spatially resolved dust gap, and an outer ring. When fitting sky-brightness models to the real component of the 3mm visibilities, we infer that the inner emission is compact (<= 1 au in radius), the gap width is between 18 and 28 au, and the emission from the outer ring peaks at similar to 36 au. We compare our ALMA image with previously published 1.6 mu m VLT/SPHERE imagery. This comparison reveals that the location of the outer ring is wavelength dependent. More specifically, the peak emission of the 3mm ring is at a larger radial distance than that of the 1.6 mu m ring, suggesting that millimeter-sized grains in the outer disc are located farther away from the central star than micron-sized grains. We discuss different scenarios to explain our findings, including dead zones, star-driven photoevaporation, and planet-disc interactions. We find that the most likely origin of the dust gap is from an embedded planet, and estimate - for a single planet scenario - that TCha's gap is carved by a 1.2M(Jup) planet.en_US
dc.description.sponsorshipNSF Astronomy & Astrophysics Research Grant [1515392]; NASA - Space Telescope Science Institute [HST-HF2-51380.001-A]; NASA [NAS 5-26555]en_US
dc.language.isoenen_US
dc.publisherOXFORD UNIV PRESSen_US
dc.relation.urlhttps://academic.oup.com/mnrasl/article/475/1/L62/4705905en_US
dc.rights© 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectplanets and satellites: detectionen_US
dc.subjectplanets and satellites: formationen_US
dc.subjectplanet-disc interactionsen_US
dc.subjectprotoplanetary discsen_US
dc.subjectcircumstellar matteren_US
dc.titleA likely planet-induced gap in the disc around T Chaen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.contributor.departmentUniv Arizona, Steward Observ, Dept Astronen_US
dc.identifier.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleMonthly Notices of the Royal Astronomical Society: Letters
dc.source.volume475
dc.source.issue1
dc.source.beginpageL62
dc.source.endpageL66
refterms.dateFOA2018-11-16T23:00:15Z


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