CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER

Johnson, John Asher; Gazak, J. Zachary; Apps, Kevin; Muirhead, Philip S.; Crepp, Justin R.; Crossfield, Ian J. M.; Boyajian, Tabetha S.; Braun, Kaspar von; Rojas-Ayala, Bárbara; Howard, Andrew W.; Covey, Kevin R.; Schlawin, Everett; Hamren, Katherine; Morton, Timothy; Marcy, Geoffrey W.; Lloyd, James P.

doi:10.1088/0004-6256/143/5/111

Cited by 168 publications

(134 citation statements)

References 88 publications

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“…We also confirm that the EGP-host metallicity correlation previously found by RV surveys (e.g. Sousa et al 2011;Johnson et al 2012;Mortier et al 2013) holds for the transit exoplanet population in the Kepler field. This suggests that similar formation processes are at work in both fields, at least for EGPs.…”

Section: Discussionsupporting

confidence: 89%

“…KOI-428 (Santerne et al 2011a), WASP-72 (Gillon et al 2013), WASP-73 (Delrez et al 2014). At the other extreme, only one EGP has been found with a transit depth greater than 3%, KOI-254 (Johnson et al 2012), whose M-dwarf host represents a small fraction of the KOIs (Dressing & Charbonneau 2013). We are therefore confident that those criteria select the majority of the EGPs transiting FGK dwarfs.…”

Section: The Giant-planet Candidate Samplementioning

confidence: 85%

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SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

A&A

259

256

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While giant extrasolar planets have been studied for more than two decades now, there are still some open questions as to their dominant formation and migration processes, as well as to their atmospheric evolution in different stellar environments. In this paper, we study a sample of giant transiting exoplanets detected by the Kepler telescope with orbital periods up to 400 days. We first defined a sample of 129 giant-planet candidates that we followed up with the SOPHIE spectrograph (OHP, France) in a 6-year radial velocity campaign. This allowed us to unveil the nature of these candidates and to measure a false-positive rate of 54.6 ± 6.5% for giant-planet candidates orbiting within 400 days of period. Based on a sample of confirmed or likely planets, we then derived the occurrence rates of giant planets in different ranges of orbital periods. The overall occurrence rate of giant planets within 400 days is 4.6 ± 0.6%. We recovered, for the first time in the Kepler data, the different populations of giant planets reported by radial velocity surveys. Comparing these rates with other yields, we find that the occurrence rate of giant planets is lower only for hot Jupiters but not for the longer-period planets. We also derive a first measurement of the occurrence rate of brown dwarfs in the brown-dwarf desert with a value of 0.29 ± 0.17%. Finally, we discuss the physical properties of the giant planets in our sample. We confirm that giant planets receiving moderate irradiation are not inflated, but we find that they are on average smaller than predicted by formation and evolution models. In this regime of low-irradiated giant planets, we find a possible correlation between their bulk density and the iron abundance of the host star, which needs more detections to be confirmed.

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Section: Discussionsupporting

confidence: 89%

Section: The Giant-planet Candidate Samplementioning

confidence: 85%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

A&A

259

256

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“…However, the Bonfils et al (2005) is also similar to Schlaufman & Laughlin (2010) and Neves et al (2012) which may explain part of the low dispersion. Regarding the Johnson et al (2012) calibration, we obtain a rms of 0.19 dex, higher that their reported value of 0.15 dex. The dispersion of the spectroscopic determinations are within the expected values (∼0.11 dex), considering the uncertainties of each method, except in the case of Mann et al (2013b), where we obtain a dispersion of 0.16 dex, and in two stars in common with Woolf & Wallerstein (2005), where the [Fe/H] difference for Gl191 and Gl526 is higher that the uncertainties reported here and in their work (0.14 and −0.12 dex, respectively).…”

Section: Comparison With the Literaturecontrasting

confidence: 68%

“…Bonfils et al 2005;Johnson & Apps 2009;Schlaufman & Laughlin 2010;Johnson et al 2012;Neves et al 2012) or spectroscopic indices (e.g. Rojas-Ayala et al 2010Mann et al 2013a,b;Newton 2013).…”

Section: Introductionmentioning

confidence: 99%

Metallicity of M dwarfs

Neves

Bonfils

Santos

et al. 2014

A&A

116

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Aims. In this work we develop a technique to obtain high precision determinations of both metallicity and effective temperature of M dwarfs in the optical. , T eff and spectral type respectively. We also calculated the RMSE V which estimates uncertainties of the order of 0.12 dex for the metallicity and of 293 K for the effective temperature. The technique has an activity limit and should only be used for stars with log L Hα /L bol < −4.0.

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“…Its orbital period is 0.81 d, the only hot Jupiter having a smaller period being . Furthermore, it orbits around a very cool K7-type dwarf that has the lowest mass among all the stars orbited by a hot Jupiter (0.58 ± 0.05 M , T eff = 4400 ± 200 K, H11), except for the recently announced M0 dwarf KOI-254 (0.59 ± 0.06 M , T eff = 3820 ± 90 K, Johnson et al 2012). Nevertheless, H11 presented another plausible solution for the stellar mass that is significantly larger, 0.71 ± 0.05 M .…”

Section: Introductionmentioning

confidence: 99%