J/ApJS/237/38 Extended abundance analysis of KOIs (Brewer+, 2018)
Spectral properties of cool stars: extended abundance analysis of Kepler Objects
of Interest.
Brewer J.M., Fischer D.A.
<Astrophys. J. Suppl. Ser., 237, 38 (2018)>
=2018ApJS..237...38B 2018ApJS..237...38B
ADC_Keywords: Abundances; Spectra, optical; Radial velocities; Stars, masses;
Rotational velocities; Stars, diameters; Stars, ages
Keywords: planetary systems ; stars: abundances ; stars: solar-type
Abstract:
Accurate stellar parameters and precise elemental abundances are vital
pieces to correctly characterize discovered planetary systems, better
understand planet formation, and trace galactic chemical evolution. We
have performed a uniform spectroscopic analysis for 1127 stars,
yielding accurate gravity, temperature, and projected rotational
velocity in addition to precise abundances for 15 elements (C, N, O,
Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Fe, Ni, and Y). Most of the stars
in this sample are Kepler Objects of Interest, observed by the
California-Kepler Survey, and include 1003 stars hosting 1562
confirmed planets. This catalog extends the uniform analysis of our
previous catalog, bringing the total number of homogeneously analyzed
stars to almost 2700 F, G, and K dwarfs. To ensure consistency between
the catalogs, we performed an analysis of our ability to recover
parameters as a function of signal-to-noise ratio (S/N) and present
individual uncertainties as well as functions to calculate
uncertainties for parameters derived from lower S/N spectra. With the
updated parameters, we used isochrone fitting to derive new radii,
masses, and ages for the stars. We use our abundance analysis to
support the finding that the radius gap is likely a result of
evolution rather than the result of primordial compositional
differences between the two populations.
Description:
The California-Kepler Survey (CKS) program (Petigura+ 2017, J/AJ/154/107)
obtained Keck HIRES spectra of a large number of KOIs using the same
instrumental setup as that in Brewer+, 2016, J/ApJS/225/32. This
allowed us to easily apply the same analysis method to derive stellar
properties and abundances for all of the stars. The CKS program
targeted the first large data release of KOIs (Borucki+ 2011,
J/ApJ/736/19), expanded that to include all KOIs with Kp<14.2, then
included some more interesting fainter systems.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 106 1149 Spectroscopically determined stellar properties
table4.dat 111 1149 Spectroscopically determined stellar
elemental abundances
table5.dat 85 1149 Derived Stellar Properties
table6.dat 112 1149 Uncertainties for spectroscopically determined
stellar properties and abundances
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/A+A/415/1153 : [Fe/H] for 98 extra-solar planet-host stars (Santos+, 2004)
J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)
J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)
J/ApJS/168/297 : Stellar parameters of nearby cool stars (Takeda+, 2007)
J/ApJ/725/875 : Chromospheric activity for CPS stars (Isaacson+, 2010)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012)
J/ApJ/771/107 : Spectroscopy of faint KOI stars (Everett+, 2013)
J/ApJ/809/8 : Terrestrial planet occurrence rates for KOIs (Burke+, 2015)
J/ApJ/815/5 : Abundances of KOI stars with planets. I. (Schuler+, 2015)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)
J/AJ/152/187 : Planet occurrence & metallicities for KOIs (Mulders+, 2016)
J/ApJ/835/173 : Kepler asteroseismic LEGACY sample. II. (Silva Aguirre+, 2017)
J/AJ/154/107 : California-Kepler Survey (CKS). I. (Petigura+, 2017)
J/AJ/154/108 : California-Kepler Survey (CKS). II. (Johnson+, 2017)
J/AJ/154/109 : CKS. III. Planet radii (Fulton+, 2017)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- SPOCS [2281/4319] SPOCS identifier (G1)
6- 20 A15 --- Name Identifier
22- 23 I2 h RAh [0/23] Hour of Right Ascension (J2000)
25- 26 I2 min RAm Minute of Right Ascension (J2000)
28- 31 F4.1 s RAs Second of Right Ascension (J2000)
33 A1 --- DE- Sign of the Declination (J2000)
34- 35 I2 deg DEd Degree of Declination (J2000)
37- 38 I2 arcmin DEm Arcminute of Declination (J2000)
40- 41 I2 arcsec DEs Arcsecond of Declination (J2000)
43- 46 I4 K Teff [4703/6748] Effective temperature
from this analysis
48- 51 F4.2 [cm/s2] log(g) [2.7/5] log surface gravity from this analysis
53- 57 F5.2 [Sun] [M/H] [-1.1/0.5] Metallicity from this analysis (1)
59- 62 F4.2 --- SHK [0/1.1] Chromospheric activity indicator SHK
64- 68 F5.2 [-] logRHK [-7.6/0]? Chromospheric activity indicator
log(RHK) (2)
70- 73 F4.1 km/s vbroad [0.8/24.9] Rotational broadening
75- 78 F4.1 km/s vsini [0/20.5] Projected rotational velocity
80- 83 F4.1 km/s vmac [1.6/15.2] Macroscopic velocity
85- 90 F6.1 km/s RVel [-143.3/54.1] Radial velocity
92- 94 I3 --- S/N [17/260] Average Signal-to-Noise at 6000Å
96- 99 F4.2 --- C-rms [0.01/0.6] RMS residuals in the continuum
regions (3)
101-104 F4.2 --- L-rms [0.01/0.1] RMS residuals in the line regions (3)
106 I1 --- N [1/3] Number of spectra analyzed
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Note (1): Note that [M/H] is the metallicity of the model atmosphere used to
derive the best fit model spectrum but does not necessarily match
the [Fe/H] value for the star.
Note (2): A blank indicates a NaN value.
Note (3): Between model and observation.
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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 I4 --- SPOCS [2281/4319] SPOCS identifier (G1)
6- 20 A15 --- Name Identifier
22- 26 F5.2 [Sun] [C/H] [-1/0.8] log C/H number abundance
28- 33 F6.2 [Sun] [N/H] [-37.5/1.2] log N/H number abundance
35- 39 F5.2 [Sun] [O/H] [-0.7/0.9] log O/H number abundance
41- 45 F5.2 [Sun] [Na/H] [-1.1/0.9] log Na/H number abundance
47- 51 F5.2 [Sun] [Mg/H] [-0.8/0.4] log Mg/H number abundance
53- 57 F5.2 [Sun] [Al/H] [-2.4/1] log Al/H number abundance
59- 63 F5.2 [Sun] [Si/H] [-0.7/0.6] log Si/H number abundance
65- 69 F5.2 [Sun] [Ca/H] [-0.8/0.9] log Ca/H number abundance
71- 75 F5.2 [Sun] [Ti/H] [-1/0.5] log Ti/H number abundance
77- 81 F5.2 [Sun] [V/H] [-1.9/0.7] log V/H number abundance
83- 87 F5.2 [Sun] [Cr/H] [-1.2/0.5] log Cr/H number abundance
89- 93 F5.2 [Sun] [Mn/H] [-1.6/0.6] log Mn/H number abundance
95- 99 F5.2 [Sun] [Fe/H] [-0.7/0.5] log Fe/H number abundance
101-105 F5.2 [Sun] [Ni/H] [-0.8/0.9] log Ni/H number abundance
107-111 F5.2 [Sun] [Y/H] [-1.4/1.2] log Y/H number abundance
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- SPOCS [2281/4319] SPOCS identifier (G1)
6- 20 A15 --- Name Identifier
22- 28 F7.4 mas plx [-3.1/27.4]? Parallax from Gaia DR2
30- 34 F5.3 mas e_plx [0.01/1]? Uncertainty in plx
36- 40 F5.2 Rsun Rad [0.6/11.8]? Radius (4)
42- 46 F5.2 Rsun b_Rad [0.6/11.6]? Lower boundary in Rad
48- 52 F5.2 Rsun B_Rad [0.6/12.1]? Upper boundary in Rad
54- 57 F4.2 Msun Mass [0.6/2.7]? Mass (4)
59- 62 F4.2 Msun b_Mass [0.6/2.7]? Lower boundary in Mass
64- 67 F4.2 Msun B_Mass [0.6/2.7]? Upper boundary in Mass
69- 73 F5.2 Gyr Age [0.3/15]? Age (4)
75- 79 F5.2 Gyr b_Age [0.2/14.9]? Lower boundary in Age
81- 85 F5.2 Gyr B_Age [0.3/15]? Upper boundary in Age
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Note (4): Stellar properties derived from Dartmouth Isochrone fitting with
python isochrones package and pyMultiNest with K magnitudes.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- SPOCS [2281,4319] SPOCS identifier (G1)
6- 20 A15 --- Name Identifier
22- 23 I2 K e_Teff [25/42] Uncertainty in effective temperature
25- 28 F4.2 [cm/s2] e_log(g) [0.05/0.08] Uncertainty in log surface gravity
30- 33 F4.2 [Sun] e_[M/H] [0.01/0.03] Uncertainty in metallicity
35- 37 F3.1 km/s e_vsini [0.5/0.7] Uncertainty in Projected rotational
velocity
39- 42 F4.2 [Sun] e_[C/H] [0.03/0.07] Uncertainty in log C/H number
abundance
44- 47 F4.2 [Sun] e_[N/H] [0.04/0.2] Uncertainty in log N/H number
abundance
49- 52 F4.2 [Sun] e_[O/H] [0.04/0.2] Uncertainty in log O/H number
abundance
54- 57 F4.2 [Sun] e_[Na/H] [0.01/0.08] Uncertainty in log Na/H
number abundance
59- 62 F4.2 [Sun] e_[Mg/H] [0.01/0.05] Uncertainty in log Mg/H number
abundance
64- 67 F4.2 [Sun] e_[Al/H] [0.03/0.1] Uncertainty in log Al/H number
abundance
69- 72 F4.2 [Sun] e_[Si/H] [0.01/0.05] Uncertainty in log Si/H number
abundance
74- 77 F4.2 [Sun] e_[Ca/H] [0.01/0.06] Uncertainty in log Ca/H number
abundance
79- 82 F4.2 [Sun] e_[Ti/H] [0.01/0.05] Uncertainty in log Ti/H number
abundance
84- 87 F4.2 [Sun] e_[V/H] [0.03/0.08] Uncertainty in log V/H number
abundance
89- 92 F4.2 [Sun] e_[Cr/H] [0.01/0.04] Uncertainty in log Cr/H number
abundance
94- 97 F4.2 [Sun] e_[Mn/H] [0.02/0.07] Uncertainty in log Mn/H number
abundance
99-102 F4.2 [Sun] e_[Fe/H] [0.01/0.04] Uncertainty in log Fe/H number
abundance
104-107 F4.2 [Sun] e_[Ni/H] [0.01/0.04] Uncertainty in log Ni/H number
abundance
109-112 F4.2 [Sun] e_[Y/H] [0.03/0.1] Uncertainty in log Y/H number
abundance
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Globale note:
Note (G1): SPOCS ID numbers are shared with the Valenti & Fischer
(2005, J/ApJ/622/1102) and Brewer+ (2016, J/ApJS/225/32)
catalogs for stars in common between those works and this. Stars new
to this catalog have an ID≥3248.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 22-Oct-2018