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    K2-291b: A Rocky Super-Earth in a 2.2 day Orbit

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    Kosiarek_2019_AJ_157_116.pdf (2.788Mb)
    Issue Date
    2019-02-13
    Author
    Kosiarek, Molly R.
    Blunt, Sarah
    López-Morales, Mercedes
    Crossfield, Ian
    Sinukoff, Evan
    Petigura, Erik A.
    Gonzales, Erica J.
    Poretti, Ennio
    Malavolta, Luca
    Howard, Andrew W.
    Isaacson, Howard
    Haywood, Raphaëlle D.
    Ciardi, David R.
    Bristow, Makennah
    Cameron, Andrew Collier
    Charbonneau, David
    Dressing, Courtney D.
    Figueira, Pedro
    Fulton, Benjamin J.
    Hardee, Bronwen J.
    Hirsch, Lea A.
    Latham, David W.
    Mortier, Annelies
    Nava, Chantanelle
    Schlieder, Joshua E.
    Vanderburg, Andrew
    Weiss, Lauren
    Bonomo, Aldo S.
    Bouchy, François
    Buchhave, Lars A.
    Coffinet, Adrien
    Damasso, Mario
    Dumusque, Xavier
    Lovis, Christophe
    Mayor, Michel
    Micela, Giusi
    Molinari, Emilio
    Pepe, Francesco
    Phillips, David
    Piotto, Giampaolo
    Rice, Ken
    Sasselov, Dimitar
    Ségransan, Damien
    Sozzetti, Alessandro
    Udry, Stéphane
    Watson, Chris
    Publisher
    IOP Publishing
    Type
    Article
    Article Version
    Scholarly/refereed, publisher version
    Rights
    © 2019. The American Astronomical Society. All rights reserved.
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    Abstract
    K2-291 is a solar-type star with a radius of R * = 0.899 ± 0.034 R ⊙ and mass of M* = 0.934 ± 0.038 M ⊙. From the K2 C13 data, we found one super-Earth planet (R p = ${1.589}_{-0.072}^{+0.095}$ R ⊕) transiting this star on a short period orbit (P = ${2.225177}_{-6.8{\rm{e}}\mbox{--}5}^{+6.6{\rm{e}}\mbox{--}5}$ days). We followed this system up with adaptive-optic imaging and spectroscopy to derive stellar parameters, search for stellar companions, and determine a planet mass. From our 75 radial velocity measurements using High Resolution Echelle Spectrometer on Keck I and High Accuracy Radial velocity Planet Searcher in the northern hemisphere on Telescopio Nazionale Galileo, we constrained the mass of K2-291 b to M p = 6.49 ± 1.16 M ⊕. We found it necessary to model correlated stellar activity radial velocity signals with a Gaussian process (GP) in order to more accurately model the effect of stellar noise on our data; the addition of the GP also improved the precision of this mass measurement. With a bulk density of ρ = 8.84${}_{-2.03}^{+2.50}$ g cm−3, the planet is consistent with an Earth-like rock/iron composition and no substantial gaseous envelope. Such an envelope, if it existed in the past, was likely eroded away by photoevaporation during the first billion years of the star's lifetime.
    URI
    http://hdl.handle.net/1808/30999
    DOI
    https://doi.org/10.3847/1538-3881/aafe83
    Collections
    • Physics & Astronomy Scholarly Works [1713]
    Citation
    Molly R. Kosiarek et al 2019 AJ 157 116

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    Contact KU ScholarWorks
    785-864-8983
    KU Libraries
    1425 Jayhawk Blvd
    Lawrence, KS 66045
    785-864-8983

    KU Libraries
    1425 Jayhawk Blvd
    Lawrence, KS 66045
    Image Credits
     

     

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