CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BY<i>KEPLER</i>. II. ANALYSIS OF THE FIRST FOUR MONTHS OF DATA

Borucki, W. J.; Koch, David; Basri, Gibor; Batalha, Natalie M.; Brown, Timothy M.; Bryson, Stephen T.; Caldwell, Douglas A.; Christensen‐Dalsgaard, J.; Cochran, William D.; DeVore, Edna; Dunham, E. W.; Gautier, T. N.; Geary, John C.; Gilliland, Ronald L.; Gould, A.; Howell, Steve B.; Jenkins, Jon M.; Latham, David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Rowe, Jason F.; Sasselov, Dimitar; Boss, Alan P.; Charbonneau, David; Ciardi, David R.; Doyle, Laurance R.; Dupree, A. K.; Ford, Eric B.; Fortney, Jonathan J.; Holman, Matthew J.; Seager, Sara; Steffen, Jason H.; Tarter, Jill; Welsh, William F.; Allen, Christopher S.; Buchhave, Lars A.; Christiansen, Jessie L.; Clarke, Bruce; Das, Santanu; Désert, Jean Michel; Endl, Michael; Fabrycky, Daniel C.; Fressin, François; Haas, Michael R.; Horch, Elliott; Howard, Andrew W.; Isaacson, Howard; Kjeldsen, H.; Kolodziejczak, Jeffery J.; Kulesa, Craig; Li, Jie; Lucas, P. W.; Machálek, Pavel; McCarthy, Donald W.; MacQueen, Phillip J.; Meibom, S.; Miquel, Thibaut; Prša, Andrej; Quinn, Samuel N.; Quintana, Elisa V.; Ragozzine, Darin; Sherry, William; Shporer, Avi; Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Cleve, Jeffrey Van; Walkowicz, Lucianne M.; Witteborn, F. C.; Still, M.

doi:10.1088/0004-637x/736/1/19

Cited by 924 publications

(799 citation statements)

References 45 publications

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“…The scientific aims of the Kepler mission were presented by Borucki et al (2003), while Borucki et al (2011) gave an early summary of results. This has been updated by Rowe et al (2014), Mulally et al (2015) and others.…”

Section: Introductionmentioning

confidence: 99%

An investigation into exoplanet transits and uncertainties

Ji¹,

Banks

Budding

et al. 2017

Astrophys Space Sci

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Section: Introductionmentioning

confidence: 99%

An investigation into exoplanet transits and uncertainties

Ji¹,

Banks

Budding

et al. 2017

Astrophys Space Sci

View full text Add to dashboard Cite

“…The NASA Kepler mission has detected thousands of planet candidates with radii between 1 and 2.7 R ⊕ (Borucki et al 2011;Batalha et al 2013;Burke et al 2014;Rowe et al 2015). The corresponding population of low mass planets was previously detected in radial velocity (RV) surveys (Mayor & Udry 2008;Howard et al 2009), but notably has no analog in our own solar system.…”

Section: Introductionmentioning

confidence: 99%

The Kepler-454 System: A Small, Not-Rocky Inner Planet, a Jovian World, and a Distant Companion

Gettel

Charbonneau

Dressing

et al. 2016

ApJ

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Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like star that hosts a transiting planet candidate in a 10.6 day orbit. From spectroscopy, we estimate the stellar temperature to be 5687±50 K, its metallicity to be [m/H] = 0.32±0.08, and the projected rotational velocity to be v sin i<2.4 km s −1 . We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be M 1.028 0.03 0.04 -+  , the radius to be 1.066±0.012 R e , and the age to be 5.25 1.39Gyr. We estimate the radius of the 10.6 day planet as 2.37±0.13 R ⊕ . Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at the Keck Observatory, we measure the mass of this planet to be 6.8±1.4 M ⊕ . We also detect two additional nontransiting companions, a planet with a minimum mass of 4.46±0.12 M J in a nearly circular 524 day orbit and a massive companion with a period >10 years and mass >12.1 M J . The 12 exoplanets with radii <2.7 R ⊕ and precise mass measurements appear to fall into two populations, with those <1.6 R ⊕ following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76±0.73 g cm −3 , Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.

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“…Most exoplanets have been found by the radial velocity (Butler et al 2006) and transit (Borucki et al 2011) methods. These methods are sensitive to low-mass planets orbiting less than 1 AU from the host star.…”

Section: Introductionmentioning

confidence: 99%

Ogle-2012-BLG-0724lb: A Saturn-Mass Planet Around an M Dwarf

Hirao

Udalski

Sumi

et al. 2016

ApJ

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We report the discovery of a planet by the microlensing method, OGLE-2012-BLG-0724Lb. Although the duration of the planetary signal for this event was one of the shortest seen for a planetary event, the anomaly was well covered thanks to high-cadence observations taken by the survey groups OGLE and MOA. By analyzing the light curve, this planetary system is found to have a mass ratio ( ) = ´-q 1.58 0.15 10 3 . By conducting a Bayesian analysis, we estimate that the host star is an M dwarf with a mass of . Because the lens-source relative proper motion is relatively high, future highresolution images would detect the lens host star and determine the lens properties uniquely. This system is likely a Saturn-mass exoplanet around an M dwarf, and such systems are commonly detected by gravitational microlensing. This adds another example of a possible pileup of sub-Jupiters ( )in contrast to a lack of Jupiters ( -M 1 2 Jup ) around M dwarfs, supporting the prediction by core accretion models that Jupitermass or more massive planets are unlikely to form around M dwarfs.

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CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BYKEPLER. II. ANALYSIS OF THE FIRST FOUR MONTHS OF DATA

Cited by 924 publications

References 45 publications

An investigation into exoplanet transits and uncertainties

An investigation into exoplanet transits and uncertainties

The Kepler-454 System: A Small, Not-Rocky Inner Planet, a Jovian World, and a Distant Companion

Ogle-2012-BLG-0724lb: A Saturn-Mass Planet Around an M Dwarf

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