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    Bright Opportunities for Atmospheric Characterization of Small Planets: Masses and Radii of K2-3 b, c, and d and GJ3470 b from Radial Velocity Measurements and Spitzer Transits

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    Issue Date
    2019-02-05
    Author
    Kosiarek, Molly R.
    Crossfield, Ian
    Hardegree-Ullman, Kevin K.
    Livingston, John H.
    Benneke, Björn
    Henry, Gregory W.
    Howard, Ward S.
    Berardo, David
    Blunt, Sarah
    Fulton, Benjamin J.
    Hirsch, Lea A.
    Howard, Andrew W.
    Isaacson, Howard
    Petigura, Erik A.
    Sinukoff, Evan
    Weiss, Lauren
    Bonfils, X.
    Dressing, Courtney D.
    Knutson, Heather A.
    Schlieder, Joshua E.
    Werner, Michael
    Gorjian, Varoujan
    Krick, Jessica
    Morales, Farisa Y.
    Astudillo-Defru, Nicola
    Almenara, J.-M.
    Delfosse, X.
    Forveille, T.
    Lovis, C.
    Mayor, M.
    Murgas, F.
    Pepe, F.
    Santos, N. C.
    Udry, S.
    Corbett, H. T.
    Fors, Octavi
    Law, Nicholas M.
    Ratzloff, Jeffrey K.
    del Ser, Daniel
    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
    We report improved masses, radii, and densities for four planets in two bright M-dwarf systems, K2-3 and GJ3470, derived from a combination of new radial velocity and transit observations. Supplementing K2 photometry with follow-up Spitzer transit observations refined the transit ephemerides of K2-3 b, c, and d by over a factor of 10. We analyze ground-based photometry from the Evryscope and Fairborn Observatory to determine the characteristic stellar activity timescales for our Gaussian Process fit, including the stellar rotation period and activity region decay timescale. The stellar rotation signals for both stars are evident in the radial velocity data and is included in our fit using a Gaussian process trained on the photometry. We find the masses of K2-3 b, K2-3 c, and GJ3470 b to be 6.48${}_{-0.93}^{+0.99}$, 2.14${}_{-1.04}^{+1.08}$, and 12.58${}_{-1.28}^{+1.31}$ M ⊕, respectively. K2-3 d was not significantly detected and has a 3σ upper limit of 2.80 M ⊕. These two systems are training cases for future TESS systems; due to the low planet densities (ρ < 3.7 g cm−3) and bright host stars (K < 9 mag), they are among the best candidates for transmission spectroscopy in order to characterize the atmospheric compositions of small planets.
    URI
    http://hdl.handle.net/1808/30997
    DOI
    https://doi.org/10.3847/1538-3881/aaf79c
    Collections
    • Physics & Astronomy Scholarly Works [1713]
    Citation
    Molly R. Kosiarek et al 2019 AJ 157 97

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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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