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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 156 1305 Stellar properties
table4.dat 106 2025 California-Kepler Survey (CKS) planet parameters
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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
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Bytes Format Units Label Explanations
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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
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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.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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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
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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 2014ApJ...789L..20D).
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History:
From electronic version of the journal
References:
Petigura et al., Paper I 2017AJ....154..107P 2017AJ....154..107P, Cat. J/AJ/154/107
Fulton et al., Paper III 2017AJ....154..109F 2017AJ....154..109F, Cat. J/AJ/154/109
Petigura et al., Paper IV 2018AJ....155...89P 2018AJ....155...89P, Cat. J/AJ/155/89
Weiss et al., Paper V 2018AJ....155...48W 2018AJ....155...48W, Cat. J/AJ/155/48
Weiss et al., Paper VI 2018AJ....156..254W 2018AJ....156..254W
Fulton & Petigura., Paper VII 2018AJ....156..264F 2018AJ....156..264F
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 14-Dec-2017