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J/AJ/154/109  California-Kepler Survey (CKS). III. Planet radii  (Fulton+, 2017)

The California-Kepler Survey. III. A gap in the radius distribution of small planets. Fulton B.J., Petigura E.A., Howard A.W., Isaacson H., Marcy G.W., Cargile P.A., Hebb L., Weiss L.M., Johnson J.A., Morton T.D., Sinukoff E., Crossfield I.J.M., Hirsch L.A. <Astron. J., 154, 109-109 (2017)> =2017AJ....154..109F (SIMBAD/NED BibCode)
ADC_Keywords: Planets Keywords: planetary systems Abstract: The size of a planet is an observable property directly connected to the physics of its formation and evolution. We used precise radius measurements from the California-Kepler Survey to study the size distribution of 2025 Kepler planets in fine detail. We detect a factor of ≥2 deficit in the occurrence rate distribution at 1.5-2.0R. This gap splits the population of close-in (P<100days) small planets into two size regimes: RP<1.5R and RP=2.0--3.0R, with few planets in between. Planets in these two regimes have nearly the same intrinsic frequency based on occurrence measurements that account for planet detection efficiencies. The paucity of planets between 1.5 and 2.0R supports the emerging picture that close-in planets smaller than Neptune are composed of rocky cores measuring 1.5R or smaller with varying amounts of low-density gas that determine their total sizes. Description: We adopt the stellar sample and the measured stellar parameters from the California-Kepler Survey (CKS) program (Petigura et al. 2017, Cat. J/AJ/154/107; Paper I). The measured values of Teff, logg, and [Fe/H] are based on a detailed spectroscopic characterization of Kepler Object of Interest (KOI) host stars using observations from Keck/HIRES. In Johnson et al. 2017 (Cat J/AJ/154/108; Paper II), we associated those stellar parameters from Paper I to Dartmouth isochrones (Dotter et al. 2008ApJS..178...89D) to derive improved stellar radii and masses, allowing us to recalculate planetary radii using the light-curve parameters from Mullally et al. 2015 (Cat. J/ApJS/217/31). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 84 900 *Planet detection statistics
Note on table2.dat: Refer to Paper II (Johnson et al. 2017, Cat. J/AJ/154/108) for the California-Kepler Survey (CKS) stellar parameters associated with each Kepler Object of Interest (KOI). This table contains only the subset of planet detections that passed the filters described in Section 2.2. The full sample of planet candidates orbiting CKS target stars can be found in Paper II.
See also: J/AJ/154/107 : California-Kepler Survey (CKS). I. (Petigura+, 2017) J/AJ/154/108 : California-Kepler Survey (CKS). II. (Johnson+, 2017) J/ApJS/217/31 : Kepler planetary candidates. VI. 4yr Q1-Q16 (Mullally+, 2015) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1 A1 --- --- [K] 2- 9 F08.2 --- KOI Kepler Object Identifier (KOI) of the candidate planet 11- 21 F11.8 d Per Kepler candidate orbital period 23- 29 E7.1 d E_Per Upper uncertainty in Per 31- 37 E7.1 d e_Per Lower uncertainty in Per 39- 43 F5.2 Rgeo Rad Candidate planet radius (Rp) 45- 48 F4.2 Rgeo E_Rad Upper uncertainty in Rad 50- 53 F4.2 Rgeo e_Rad Lower uncertainty in Rad 55- 61 F7.2 --- S/N Transit signal-to-noise ratio (mi) 63- 67 F5.3 --- DProb Detection probability (Pdet) 69- 74 F6.4 --- TProb Transit probability 76- 84 F9.2 --- Weight Mean total search completeness (1/wi)
History: From electronic version of the journal References: Petigura et al., Paper I 2017AJ....154..107P, Cat. J/AJ/154/107 Johnson et al., Paper II 2017AJ....154..108J, Cat. J/AJ/154/108
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 21-Dec-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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