The Kepler-19 System: A Transiting 2.2 R-Circle Plus Planet And A Second Planet Detected Via Transit Timing Variations

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dc.contributor.utaustinauthorCochran, William D.en_US
dc.contributor.utaustinauthorEndl, Michaelen_US
dc.creatorBallard, Sarahen_US
dc.creatorFabrycky, Danielen_US
dc.creatorFressin, Francoisen_US
dc.creatorCharbonneau, Daviden_US
dc.creatorDesert, Jean-Michelen_US
dc.creatorTorres, Guillermoen_US
dc.creatorMarcy, Geoffreyen_US
dc.creatorBurke, Christopher J.en_US
dc.creatorIsaacson, Howarden_US
dc.creatorHenze, Christopheren_US
dc.creatorSteffen, Jason H.en_US
dc.creatorCiardi, David R.en_US
dc.creatorHowell, Steven B.en_US
dc.creatorCochran, William D.en_US
dc.creatorEndl, Michaelen_US
dc.creatorBryson, Stephen T.en_US
dc.creatorRowe, Jason F.en_US
dc.creatorHolman, Matthew J.en_US
dc.creatorLissauer, Jack J.en_US
dc.creatorJenkins, Jon M.en_US
dc.creatorStill, Martinen_US
dc.creatorFord, Eric B.en_US
dc.creatorChristiansen, Jessie L.en_US
dc.creatorMiddour, Christopher K.en_US
dc.creatorHaas, Michael R.en_US
dc.creatorLi, Jieen_US
dc.creatorHall, Jennifer R.en_US
dc.creatorMcCauliff, Seanen_US
dc.creatorBatalha, Natalie M.en_US
dc.creatorKoch, David G.en_US
dc.creatorBorucki, William J.en_US
dc.date.accessioned2016-04-28T19:36:36Z
dc.date.available2016-04-28T19:36:36Z
dc.date.issued2011-12en
dc.description.abstractWe present the discovery of the Kepler-19 planetary system, which we first identified from a 9.3 day periodic transit signal in the Kepler photometry. From high-resolution spectroscopy of the star, we find a stellar effective temperature T-eff = 5541 +/- 60 K, a metallicity [Fe/H] = -0.13 +/- 0.06, and a surface gravity log(g) = 4.59 +/- 0.10. We combine the estimate of T-eff and [Fe/H] with an estimate of the stellar density derived from the photometric light curve to deduce a stellar mass of M-star = 0.936 +/- 0.040 M-circle dot and a stellar radius of R-star = 0.850 +/- 0.018 R-circle dot (these errors do not include uncertainties in the stellar models). We rule out the possibility that the transits result from an astrophysical false positive by first identifying the subset of stellar blends that reproduce the precise shape of the light curve. Using the additional constraints from the measured color of the system, the absence of a secondary source in the high-resolution spectrum, and the absence of a secondary source in the adaptive optics imaging, we conclude that the planetary scenario is more than three orders of magnitude more likely than a blend. The blend scenario is independently disfavored by the achromaticity of the transit: we measure a transit depth with Spitzer at 4.5 mu m of 547(-110)(+113) ppm, consistent with the depth measured in the Kepler optical bandpass of 567 +/- 6 ppm (corrected for stellar limb darkening). We determine a physical radius of the planet Kepler-19b of R-p = 2.209 +/- 0.048 R-circle plus; the uncertainty is dominated by uncertainty in the stellar parameters. From radial velocity observations of the star, we find an upper limit on the planet mass of 20.3 M-circle plus, corresponding to a maximum density of 10.4 g cm(-3). We report a significant sinusoidal deviation of the transit times from a predicted linear ephemeris, which we conclude is due to an additional perturbing body in the system. We cannot uniquely determine the orbital parameters of the perturber, as various dynamical mechanisms match the amplitude, period, and shape of the transit timing signal and satisfy the host star's radial velocity limits. However, the perturber in these mechanisms has a period less than or similar to 160 days and mass less than or similar to 6 M-Jup, confirming its planetary nature as Kepler-19c. We place limits on the presence of transits of Kepler-19c in the available Kepler data.en_US
dc.description.departmentMcDonald Observatoryen_US
dc.description.sponsorshipNASAen_US
dc.description.sponsorshipW. M. Keck Foundationen_US
dc.identifierdoi:10.15781/T2182W
dc.identifier.Filename2011_12_kepler19.pdfen_US
dc.identifier.citationLissauer, Jack J., Rebekah I. Dawson, and Scott Tremaine. "Advances in exoplanet science from Kepler." Nature, Vol. 513, No. 7518 (Dec., 2014): 336-344.en_US
dc.identifier.doi10.1088/0004-637x/743/2/200en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34896
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journalen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.rights.restrictionOpenen_US
dc.subjecteclipsesen_US
dc.subjectplanetary systemsen_US
dc.subjectstars: individual (kepler-19, koi-84, kicen_US
dc.subject2571238)en_US
dc.subjectearth gj 1214ben_US
dc.subject1st 4 monthsen_US
dc.subjectlight curvesen_US
dc.subjectterrestrial planetsen_US
dc.subjectextrasolar planetsen_US
dc.subjectbinary starsen_US
dc.subjectinitial characteristicsen_US
dc.subjecttransmissionen_US
dc.subjectspectrumen_US
dc.subjectperiod variationsen_US
dc.subjectfalse positivesen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Kepler-19 System: A Transiting 2.2 R-Circle Plus Planet And A Second Planet Detected Via Transit Timing Variationsen_US
dc.typeArticleen_US

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