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dc.contributor.authorFaramaz, Virginie
dc.contributor.authorKrist, John
dc.contributor.authorStapelfeldt, Karl R.
dc.contributor.authorBryden, Geoffrey
dc.contributor.authorMamajek, Eric E.
dc.contributor.authorMatrà, Luca
dc.contributor.authorBooth, Mark
dc.contributor.authorFlaherty, Kevin
dc.contributor.authorHales, Antonio S.
dc.contributor.authorHughes, A. Meredith
dc.contributor.authorBayo, Amelia
dc.contributor.authorCasassus, Simon
dc.contributor.authorCuadra, Jorge
dc.contributor.authorOlofsson, Johan
dc.contributor.authorSu, Kate Y. L.
dc.contributor.authorWilner, David J.
dc.date.accessioned2019-10-24T23:03:13Z
dc.date.available2019-10-24T23:03:13Z
dc.date.issued2019-09-27
dc.identifier.citationVirginie Faramaz et al 2019 AJ 158 162en_US
dc.identifier.issn0004-6256
dc.identifier.doi10.3847/1538-3881/ab3ec1
dc.identifier.urihttp://hdl.handle.net/10150/634824
dc.description.abstractWe present here new observations of the eccentric debris ring surrounding the Gyr-old solar-type star HD 202628: at millimeter wavelengths with ALMA, at far-infrared wavelengths with Herschel, and in scattered light with the Hubble Space Telescope (HST). The ring inner edge is found to be consistent between ALMA and HST data. As radiation pressure affects small grains seen in scattered-light, the ring appears broader at optical than at millimeter wavelengths. The best fit to the ring seen with ALMA has inner and outer edges at 143.1 +/- 1.7 au and 165.5 +/- 1.4, respectively, and an inclination of 57 degrees.4 +/- 0.4 from face-on. The offset of the ring center of symmetry from the star allows us to quantify its eccentricity to be e = 0.09(-0.01)(+0.02). This eccentric feature is also detected in low resolution Herschel/PACS observations, under the form of a pericenter-glow. Combining the infrared and millimeter photometry, we retrieve a disk grain size distribution index of similar to-3.4, and therefore exclude in situ formation of the inferred belt-shaping perturber, for which we provide new dynamical constraints. Finally, ALMA images show four point-like sources that exceed 100 mu Jy, one of them being just interior to the ring. Although the presence of a background object cannot be excluded, we cannot exclude either that this source is circumplanetary material surrounding the belt-shaper, in which case degeneracies between its mass and orbital parameters could be lifted, allowing us to fully characterize such a distant planet in this mass and age regime for the very first time.en_US
dc.description.sponsorshipExoplanet Science Initiative at the Jet Propulsion Laboratory; California Inst. of Technology; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); Deutsche Forschungsgemeinschaft (DFG)German Research Foundation (DFG) [Kr 2164/15-1]; ICM (Iniciativa Cientifica Milenio) via the Nucleo Milenio de Formacion Planetaria grant; Universidad de Valparaiso; FondecytComision Nacional de Investigacion Cientifica y Tecnologica (CONICYT)CONICYT FONDECYT [1180395]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectcircumstellar matteren_US
dc.subjectplanetary systemsen_US
dc.titleFrom Scattered-light to Millimeter Emission: A Comprehensive View of the Gigayear-old System of HD 202628 and its Eccentric Debris Ringen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTRONOMICAL 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.volume158
dc.source.issue4
dc.source.beginpage162
refterms.dateFOA2019-10-24T23:03:14Z


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