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    Searching for Planets Orbiting α Cen A with the James Webb Space Telescope

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    1910.09709.pdf
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    Author
    Beichman, Charles
    Ygouf, Marie
    Sayson, Jorge Llop
    Mawet, Dimitri cc
    Yung, Yuk
    Choquet, Elodie
    Kervella, Pierre
    Boccaletti, Anthony
    Belikov, Ruslan
    Lissauer, Jack J.
    Quarles, Billy
    Lagage, Pierre-Olivier
    Dicken, Daniel
    Hu, Renyu
    Mennesson, Bertrand
    Ressler, Mike
    Serabyn, Eugene
    Krist, John
    Bendek, Eduardo
    Leisenring, Jarron
    Pueyo, Laurent
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2020-01
    Keywords
    infrared
    planetary systems planetary systems planets and satellites
    detection space vehicles
    instruments
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Charles Beichman et al 2020 PASP 132 015002
    Journal
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
    Rights
    © 2019. The Astronomical Society of the Pacific. All rights reserved.
    Collection Information
    This 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.
    Abstract
    a 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.
    Note
    12 month embargo; published online: 12 December 2019
    ISSN
    0004-6280
    EISSN
    1538-3873
    DOI
    10.1088/1538-3873/ab5066
    Version
    Final accepted manuscript
    Sponsors
    Jet Propulsion Laboratory
    ae974a485f413a2113503eed53cd6c53
    10.1088/1538-3873/ab5066
    Scopus Count
    Collections
    UA Faculty Publications

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