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dc.contributor.authorSepulveda, Aldo G.
dc.contributor.authorMatrà, Luca
dc.contributor.authorKennedy, Grant M.
dc.contributor.authorBurgo, Carlos del
dc.contributor.authorÖberg, Karin I.
dc.contributor.authorWilner, David J.
dc.contributor.authorMarino, Sebastián
dc.contributor.authorBooth, Mark
dc.contributor.authorCarpenter, John M.
dc.contributor.authorDavies, Claire L.
dc.contributor.authorDent, William R. F.
dc.contributor.authorErtel, Steve
dc.contributor.authorLestrade, Jean-Francois
dc.contributor.authorMarshall, Jonathan P.
dc.contributor.authorMilli, Julien
dc.contributor.authorWyatt, Mark C.
dc.contributor.authorMacGregor, Meredith A.
dc.contributor.authorMatthews, Brenda C.
dc.date.accessioned2019-09-26T00:01:37Z
dc.date.available2019-09-26T00:01:37Z
dc.date.issued2019-08-14
dc.identifier.citationAldo G. Sepulveda et al 2019 ApJ 881 84en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab2b98
dc.identifier.urihttp://hdl.handle.net/10150/634591
dc.description.abstractDebris disks are extrasolar analogs to our own Kuiper Belt and they are detected around at least 17% of nearby Sun-like stars. The morphology and dynamics of a disk encode information about its history, as well as that of any exoplanets within the system. We used the Atacama Large Millimeter/submillimeter Array (ALMA) to obtain 1.3 mm observations of the debris disk around the nearby F5V star HD 170773. We image the face-on ring and determine its fundamental parameters by forward-modeling the interferometric visibilities through a Markov Chain Monte Carlo approach. Using a symmetric Gaussian surface density profile, we find a 71 ± 4 au wide belt with a radius of ${193}_{-3}^{+2}$ au, a relatively large radius compared with most other millimeter-resolved belts around late A/early F type stars. This makes HD 170773 part of a group of four disks around A and F stars with radii larger than expected from the recently reported planetesimal belt radius—stellar luminosity relation. Two of these systems are known to host directly imaged giant planets, which may point to a connection between large belts and the presence of long-period giant planets. We also set upper limits on the presence of CO and CN gas in the system, which imply that the exocomets that constitute this belt have CO and HCN ice mass fractions of <77% and <3%, respectively. This is consistent with solar system comets and other exocometary belts.en_US
dc.description.sponsorshipSAO REU program - National Science Foundation REU; Department of Defense ASSURE programs under NSF [AST-1659473]; Smithsonian Institution; Mexican national council for science and technology (CONACYT grant CVU) [448248]; Deutsche Forschungsgemeinschaft [Kr 2164/15-1]; National Aeronautics and Space Administration [15XRP15_20140]; ERC Starting Grant "ImagePlanetFormDiscs" [639889]; Ministry of Science and Technology of Taiwan [MOST104-2628-M001-004-MY3, MOST107-2119-M-001-031-MY3]; Academia Sinica [AS-IA-106-M03]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectcircumstellar matteren_US
dc.subjectplanet-disk interactionsen_US
dc.subjectstars: individual (HD 170773)en_US
dc.subjecttechniques: interferometricen_US
dc.titleThe REASONS Survey: Resolved Millimeter Observations of a Large Debris Disk around the Nearby F Star HD 170773en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_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.volume881
dc.source.issue1
dc.source.beginpage84
refterms.dateFOA2019-09-26T00:01:38Z


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