<i>KEPLER</i>
                    MISSION STELLAR AND INSTRUMENT NOISE PROPERTIES

Gilliland, Ronald L.; Chaplin, W. J.; Dunham, E. W.; Argabright, Vic S.; Borucki, W. J.; Basri, Gibor; Bryson, Stephen T.; Buzasi, Derek L.; Caldwell, Douglas A.; Elsworth, Y.; Jenkins, Jon M.; Koch, David; Kolodziejczak, J.; Miglio, A.; Cleve, Jeffrey Van; Walkowicz, Lucianne M.; Welsh, William F.

doi:10.1088/0067-0049/197/1/6

Cited by 234 publications

(239 citation statements)

References 69 publications

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“…Our derived values are similar to the ones reported in the KIC, but here we can determine their uncertainties. The derived jitter is around 100 ppm for KOI-200, which is compatible with the typical value derived by Gilliland et al (2011) for the Kepler data ). In the case of KOI-889 we found ∼300 ppm; the excess of jitter could be explained by the activity of the star.…”

Section: Resultssupporting

confidence: 89%

KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

Hébrard¹,

Almenara²,

Santerne³

et al. 2013

A&A

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We present the detection and characterization of the two new transiting, close-in, giant extrasolar planets KOI-200 b and KOI-889 b. They were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite; we then established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N. Combined analyses of the whole datasets allow the two planetary systems to be characterized. The planet KOI-200 b has mass and radius of 0.68 ± 0.09 M Jup and 1.32 ± 0.14 R Jup ; it orbits in 7.34 days a F8V host star with mass and radius of 1.40 +0.14 −0.11 M and 1.51 ± 0.14 R . The planet KOI-889 b is a massive planet with mass and radius of 9.9 ± 0.5 M Jup and 1.03 ± 0.06 R Jup ; it orbits in 8.88 days an active G8V star with a rotation period of 19.2 ± 0.3 days, and mass and radius of 0.88 ± 0.06 M and 0.88 ± 0.04 R . Both planets lie on eccentric orbits and are located just at the frontier between regimes where tides can explain circularization and where tidal effects are negligible. The two planets are among the first detected and characterized thanks to observations secured with HARPS-N, the new spectrograph recently mounted at the Telescopio Nazionale Galileo. These results illustrate the benefits that could be obtained from joint studies using two spectrographs as SOPHIE and HARPS-N.

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Section: Resultssupporting

confidence: 89%

KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

Hébrard¹,

Almenara²,

Santerne³

et al. 2013

A&A

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“…Photometric accuracy is related to the position of a stellar image on this array, but for a mean flux count of about 186000 per minute for a mag 12.0 star (cf. Table 2, below) a measuring standard deviation equivalent to about 383 ppm was estimated by the Kepler Mission engineers (Gilliland et al, 2011). This is close to our finding from the best fitting models pursued in this paper, although certain examples appear to show a wider deviation, for reasons we consider later.…”

Section: Introductionsupporting

confidence: 85%

“…There are anomalies in some instances, however. The ∆l K values take some account of variation in intrinsic scatter in the source counts at a given mean brightness (Gilliland et al 2011), but if this is higher than normal in a particular case, an additional intrinsic variability, perhaps of a pulsational type, could be the explanation. This seems feasible for KOI 10.01, where there is an unexpectedly high χ 2 /ν ratio, as well as a significant excess of ∆l K /∆l p .…”

Section: Resultsmentioning

confidence: 99%

Analysis of selected Kepler Mission planetary light curves

Rhodes

Budding

2014

Astrophys Space Sci

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We have modified the graphical user interfaced close binary system analysis program CurveFit to the form WinKepler and applied it to 16 representative planetary candidate light curves found in the NASA Exoplanet Archive (NEA) at the Caltech website http://exoplanetarchive.ipac.caltech.edu, with an aim to compare different analytical approaches. WinKepler has parameter options for a realistic physical model, including gravity-brightening and structural parameters derived from the relevant Radau equation. We tested our best-fitting parameter-sets for formal determinacy and adequacy.A primary aim is to compare our parameters with those listed in the NEA. Although there are trends of agreement, small differences in the main parameter values are found in some cases, and there may be some relative bias towards a 90 • value for the NEA inclinations. These are assessed against realistic error estimates.Photometric variability from causes other than planetary transits affects at least 6 of the data-sets studied; with small pulsational behaviour found in 3 of those. For the false positive KOI 4.01, we found that the eclipses could be modelled by a faint background clas- Our empirical checks of limb-darkening, in the cases of KOI 1.01 and 12.01, revealed that the assigned stellar temperatures are probably incorrect. For KOI 13.01, our empirical mass-ratio differs by about 7% from that of Mislis and Hodgkin (Mon. Not. R. Astron. Soc. 422:1512Soc. 422: ,2012, who neglected structural effects and higher order terms in the tidal distortion. Such detailed parameter evaluation, additional to the usual main geometric ones, provides an additional objective for this work.

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“…The photometric residuals show an rms of 177 ppm, consistent with the median error of the data points (185 ppm). The rms over 3 h is 72 ppm, in agreement with the combined differential photometric precision of ∼85 ppm (Gilliland et al, 2011) provided by the Kepler team.…”

Section: L6 Page 2 Ofsupporting

confidence: 81%

SOPHIE velocimetry ofKeplertransit candidates

Moutou

Bonomo

Bruno

et al. 2013

A&A

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We report the discovery of a long-period brown-dwarf transiting companion of the solar-type star KOI-415. The transits were detected by the Kepler space telescope. We conducted Doppler measurements using the SOPHIE spectrograph at the Observatoire de HauteProvence. The photometric and spectroscopic signals allow us to characterize a 62.14 ± 2.69 M Jup brown-dwarf companion of an evolved 0.94 ± 0.06 M star in a highly eccentric orbit of P = 166.78805 ± 0.00022 days and e = 0.698 ± 0.002. The radius of KOI-415 b is 0.79 +0.12 −0.07 R Jup , a value that is compatible with theoretical predictions for a 10 Gyr, low-metallicity and non-irradiated object.

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KEPLER MISSION STELLAR AND INSTRUMENT NOISE PROPERTIES

Cited by 234 publications

References 69 publications

KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

Analysis of selected Kepler Mission planetary light curves

SOPHIE velocimetry ofKeplertransit candidates

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