J/AJ/154/108 California-Kepler Survey (CKS). II. Properties (Johnson+, 2017)
The California-Kepler Survey. II. Precise physical properties of 2025 Kepler planets and their host stars. Johnson J.A., Petigura E.A., Fulton B.J., Marcy G.W., Howard A.W., Isaacson H., Hebb L., Cargile P.A., Morton T.D., Weiss L.M., Winn J.N., Rogers L.A., Sinukoff E., Hirsch L.A. <Astron. J., 154, 108-108 (2017)> =2017AJ....154..108J (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Stars, ages ; Stars, masses ; Stars, diameters ; Effective temperatures ; Parallaxes, trigonometric ; Abundances, [Fe/H] Keywords: planets and satellites: fundamental parameters - planets and satellites: general - stars: abundances - stars: fundamental parameters - techniques: spectroscopic Abstract: We present stellar and planetary properties for 1305 Kepler Objects of Interest hosting 2025 planet candidates observed as part of the California-Kepler Survey. We combine spectroscopic constraints, presented in Paper I, with stellar interior modeling to estimate stellar masses, radii, and ages. Stellar radii are typically constrained to 11%, compared to 40% when only photometric constraints are used. Stellar masses are constrained to 4%, and ages are constrained to 30%. We verify the integrity of the stellar parameters through comparisons with asteroseismic studies and Gaia parallaxes. We also recompute planetary radii for 2025 planet candidates. Because knowledge of planetary radii is often limited by uncertainties in stellar size, we improve the uncertainties in planet radii from typically 42% to 12%. We also leverage improved knowledge of stellar effective temperature to recompute incident stellar fluxes for the planets, now precise to 21%, compared to a factor of two when derived from photometry. Description: The California-Kepler Survey (CKS) project and goals are described in detail in Paper I (Petigura et al. 2017, Cat. J/AJ/154/107) of this series. In brief, between 2012 and 2015, we obtained high-resolution (R∼50000) spectra of 1305 stars identified as Kepler Objects of Interest (KOIs) with Keck/HIRES. We used an exposure meter to achieve a uniform signal-to-noise ratio ∼45 per HIRES pixel on blaze near 5500Å. Using these spectra, we derived effective temperature (Teff), surface gravity (logg), metallicity ([Fe/H]), and projected stellar rotation velocity (vsini). In this work, we convert the observed spectroscopic properties of Paper I (Petigura et al. 2017, Cat. J/AJ/154/107) into physical stellar and planetary properties. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 156 1305 Stellar properties table4.dat 106 2025 California-Kepler Survey (CKS) planet parameters
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) I/259 : The Tycho-2 Catalogue (Hog+ 2000) J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars (Petigura+, 2017) J/ApJ/806/183 : Planet radii of Kepler Object of Interest (Wolfgang+, 2015) J/ApJS/217/31 : Kepler planetary candidates. VI. 4yr Q1-Q16 (Mullally+, 2015) J/ApJS/211/2 : Revised stellar prop. of Q1-16 Kepler targets (Huber+, 2014) J/ApJS/210/20 : Small Kepler planets radial velocities (Marcy+, 2014) J/ApJ/790/146 : Planets in Kepler's multi-transiting systems (Fabrycky+, 2014) J/ApJ/738/170 : False positive Kepler planet candidates (Morton+, 2011) J/ApJS/197/8 : Kepler's multiple transiting planets (Lissauer+, 2011) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Star name: mostly Kepler Object Identifier (KOI), or Kepler Input Calalog (KIC) number 14- 16 A3 --- --- [TYC] 18- 28 A11 --- TYC2 Tycho-2 catalog identifier 30- 33 F4.1 --- Ksmag [6.5/14.7] Apparent 2MASS Ks band magnitude 35- 38 I4 K Teff [4619/6651] Isochrones derived effective temperature (Teff,iso) (1) 40- 42 I3 K e_Teff [49/192] Lower uncertainty in Teff 44- 46 I3 K E_Teff [48/182] Upper uncertainty in Teff 48- 51 F4.2 [cm/s2] logg [2.7/4.7] Isochrones derived log surface gravity (loggiso) (1) 53- 56 F4.2 [cm/s2] e_logg [0.02/0.33] Lower uncertainty in logg 58- 61 F4.2 [cm/s2] E_logg [0.02/0.15] Upper uncertainty in logg 63- 67 F5.2 [Sun] [Fe/H] [-0.6/0.5] Isochrones derived metallicity ([Fe/H]iso) (1) 69- 72 F4.2 [Sun] e_[Fe/H] [0.01/0.1] Lower uncertainty in [Fe/H] 74- 77 F4.2 [Sun] E_[Fe/H] [0.01/0.19] Upper uncertainty in [Fe/H] 79- 82 F4.2 Msun Mass [0.6/2.2] Isochrones derived stellar mass (M*) (1) 84- 87 F4.2 Msun e_Mass [0.02/0.23] Lower uncertainty in Mass 89- 92 F4.2 Msun E_Mass [0.02/0.2] Upper uncertainty in Mass 94- 98 F5.2 Rsun Rad [0.6/10.4] Isochrones derived stellar radius (R*) (1) 100-103 F4.2 Rsun e_Rad [0.02/1.6] Lower uncertainty in Rad 105-108 F4.2 Rsun E_Rad [0.02/4.6] Upper uncertainty in Rad 110-114 F5.2 [yr] logA [8.9/10.2] Isochrones derived log age (log10(age)) (1) 116-119 F4.2 [yr] e_logA [0.05/0.56] Lower uncertainty in logA 121-124 F4.2 [yr] E_logA [0.04/0.35] Upper uncertainty in logA 126-130 F5.2 mas plx1 [0.1/35] Isochrones derived parallax (1) 132-135 F4.2 mas e_plx1 [0.01/1.4] Lower uncertainty in plx1 137-140 F4.2 mas E_plx1 [0.01/1.6] Upper uncertainty in plx1 142-146 F5.2 mas plx2 [1/15.3]? Tycho-Gaia Astrometric Solution trigonometric parallax 148-151 F4.2 mas e_plx2 [0.2/1]? Lower uncertainty in plx2 153-156 F4.2 mas E_plx2 [0.2/1]? Upper uncertainty in plx2
Note (1): We used the isochrones Python package to derive the following physical parameters: Teff, logg, [Fe/H], Mass, Rad, logA, and plx1. Isochrones returns posterior distributions on effective temperature, surface gravity, and metallicity, which are distinguished from the purely spectroscopic measurements.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [KOI-] 5- 12 F08.2 --- KOI Kepler Object Identifier (KOI) of the planet candidate 14- 20 F7.2 d Per Orbital period 22- 30 F9.6 --- Rp/R* ? Planetary to stellar radii ratio (1) 32- 40 F9.6 --- e_Rp/R* ? Lower uncertainty in Rp/R* 42- 50 F9.6 --- E_Rp/R* ? Upper uncertainty in Rp/R* 52- 59 F8.2 Rgeo Rad ? Planetary radius Rp 61- 68 F8.2 Rgeo e_Rad ? Lower uncertainty in Rad 70- 77 F8.2 Rgeo E_Rad ? Upper uncertainty in Rad 79- 83 I5 Earth Sinc ? Stellar irradiance (incident stellar flux) Sinc (2) 85- 88 I4 Earth e_Sinc ? Lower uncertainty in Sinc 90- 93 I4 Earth E_Sinc ? Upper uncertainty in Sinc 95- 98 I4 K Teq ? Equilibrium temperature Teq (3) 100-102 I3 K e_Teq ? Lower uncertainty in Teq 104-106 I3 K E_Teq ? Upper uncertainty in Teq
Note (1): From the NASA's Exoplanet Archive Q1-Q16 KOI catalog (Mullally et al. 2015, Cat. J/ApJS/217/31). Note (2): Stellar irradiance received at the planet relative to the Earth. We compute the incident flux as: Sinc/S⊕=(Teff/5778K)4(R*/R☉)2(a/au)-2, Eq. (3). Note (3): Defined according to (Teq/280K)=(Sinc/S⊕)1/4(1-α/4)1/4, Eq. (4). Assuming a Bond albedo α of 0.3, typical for super-Earth-size planets (Demory 2014ApJ...789L..20D).
History: From electronic version of the journal References: Petigura et al., Paper I 2017AJ....154..107P, Cat. J/AJ/154/107 Fulton et al., Paper III 2017AJ....154..109F, Cat. J/AJ/154/109
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 14-Dec-2017
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