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dc.contributor.authorBeichman, Charles
dc.contributor.authorYgouf, Marie
dc.contributor.authorSayson, Jorge Llop
dc.contributor.authorMawet, Dimitri
dc.contributor.authorYung, Yuk
dc.contributor.authorChoquet, Elodie
dc.contributor.authorKervella, Pierre
dc.contributor.authorBoccaletti, Anthony
dc.contributor.authorBelikov, Ruslan
dc.contributor.authorLissauer, Jack J.
dc.contributor.authorQuarles, Billy
dc.contributor.authorLagage, Pierre-Olivier
dc.contributor.authorDicken, Daniel
dc.contributor.authorHu, Renyu
dc.contributor.authorMennesson, Bertrand
dc.contributor.authorRessler, Mike
dc.contributor.authorSerabyn, Eugene
dc.contributor.authorKrist, John
dc.contributor.authorBendek, Eduardo
dc.contributor.authorLeisenring, Jarron
dc.contributor.authorPueyo, Laurent
dc.date.accessioned2020-05-28T20:11:22Z
dc.date.available2020-05-28T20:11:22Z
dc.date.issued2020-01
dc.identifier.citationCharles Beichman et al 2020 PASP 132 015002en_US
dc.identifier.issn0004-6280
dc.identifier.doi10.1088/1538-3873/ab5066
dc.identifier.urihttp://hdl.handle.net/10150/641478
dc.description.abstracta Centauri A is the closest solar-type star to the Sun and offers an excellent opportunity to detect the thermal emission of a mature planet heated by its host star. The MIRI coronagraph on the James Webb Space Telescope can search the 1-3 au (1"-2") region around a Cen A which is predicted to be stable within the a Cen AB system. We demonstrate that with reasonable performance of the telescope and instrument, a 20 hr program combining on-target and reference star observations at 15.5 pm could detect thermal emission from planets as small as 5 R. Multiple visits every 3-6 months would increase the geometrical completeness, provide astrometric confirmation of detected sources, and push the radius limit down to 3 R. An exozodiacal cloud only a few times brighter than our own should also be detectable, although a sufficiently bright cloud might obscure any planet present in the system. While current precision radial velocity (PRV) observations set a limit of 50-100 Mjs, at 1-3 au for planets orbiting a Cen A, there is a broad range of exoplanet radii up to 10 Rjs, consistent with these mass limits. A carefully planned observing sequence along with state-of-the-art postprocessing analysis could reject the light from a Cen A at the level of 10-5 at 1"-2" and minimize the influence of a Cen B located 7"-8" away in the 2022-2023 timeframe. These space-based observations would complement on-going imaging experiments at shorter wavelengths as well as PRV and astrometric experiments to detect planets dynamically. Planetary demographics suggest that the likelihood of directly imaging a planet whose mass and orbit are consistent with present PRV limits is small, 5%, and possibly lower if the presence of a binary companion further reduces occurrence rates. However, at a distance of just 1.34 pc, a Cen A is our closest sibling star and certainly merits close scrutiny.en_US
dc.description.sponsorshipJet Propulsion Laboratoryen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rights© 2019. The Astronomical Society of the Pacific. All rights reserved.en_US
dc.rights.urihttp://iopscience.iop.org/info/page/text-and-data-miningen_US
dc.subjectinfrareden_US
dc.subjectplanetary systems planetary systems planets and satellitesen_US
dc.subjectdetection space vehiclesen_US
dc.subjectinstrumentsen_US
dc.titleSearching for Planets Orbiting α Cen A with the James Webb Space Telescopeen_US
dc.typeArticleen_US
dc.identifier.eissn1538-3873
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalPUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFICen_US
dc.description.note12 month embargo; published online: 12 December 2019en_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 accepted manuscripten_US
dc.source.journaltitlePublications of the Astronomical Society of the Pacific
dc.source.volume132
dc.source.issue1007
dc.source.beginpage015002


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