J/ApJ/920/19 Spectroscopic analysis of CKS. II. Metallicities (Ghezzi+, 2021)
A Spectroscopic Analysis of the California-Kepler Survey Sample.
II. Correlations of Stellar Metallicities with Planetary Architectures.
Ghezzi L., Martinez C.F., Wilson R.F., Cunha K., Smith V.V.,
Majewski S.R.
<Astrophys. J., 920, 19 (2021)>
=2021ApJ...920...19G 2021ApJ...920...19G
ADC_Keywords: Stars, variable; Spectra, optical; Abundances, [Fe/H]
Keywords: Fundamental parameters of stars ; Planetary system formation ;
High resolution spectroscopy ; Stellar atmospheres ; Stellar
abundances
Abstract:
We present independent and self-consistent metallicities for a sample
of 807 planet-hosting stars from the California-Kepler Survey from an
LTE spectroscopic analysis using a selected sample of FeI and FeII
lines. Correlations between host-star metallicities, planet radii, and
planetary architecture (orbital periods-warm or hot-and
multiplicity-single or multiple) were investigated using nonparametric
statistical tests. In addition to confirming previous results from the
literature, e.g., that overall host-star metallicity distributions
differ between hot and warm planetary systems of all types, we report
on a new finding: when comparing the median metallicities of hot
versus warm systems, the difference for multiple super-Earths is
considerably larger when compared to that difference in single
super-Earths. The metallicity cumulative distribution functions of hot
single super-Earths versus warm single super-Earths indicate different
parent stellar populations, while for sub-Neptunes this is not the
case. The transition radius between sub-Neptunes and sub-Saturns was
examined by comparing the APOGEE metallicity distribution for the
Milky Way thin disk in the solar neighborhood with metallicity
distributions of host stars segregated based upon the largest known
planet in their system. These comparisons reveal increasingly
different metallicity distributions as the radius of the largest
planet in the systems increases, with the parent stellar metallicities
becoming significantly different for Rp>2.7R⊕. The behavior of
the p-values as a function of planet radius undergoes a large slope
change at Rp=4.4±0.5R⊕, indicating the radius boundary
between small and large planets.
Description:
The sample and data analyzed in this work are the same as in Paper I
(Martinez+, 2019, J/ApJ/875/29).
The California-Kepler Survey (CKS) team obtained high-resolution
spectra for the target stars with the High Resolution Echelle
Spectrometer (HIRES) spectrograph on the Keck I 10m telescope
(Maunakea, Hawaii). We analyzed their reduced spectra, which are
publicly available. The resolution of the HIRES spectra analyzed is
R∼60000, and the wavelength coverage is almost complete in the
interval 3640Å-7990Å. The signal-to-noise ratios (S/Ns) per
resolution element of the spectra for targets in our complete sample
range from ∼10 to ∼300, with a median value of ∼60.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 52 142032 Equivalent widths and individual Fe abundances
table2.dat 18 807 Stellar metallicities
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See also:
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/A+A/487/373 : Spectroscopic parameters of 451 HARPS-GTO stars (Sousa+, 2008)
J/ApJ/720/1290 : Abundances of stars hosting planets (Ghezzi+, 2010)
J/A+A/533/A141 : Stellar parameters for 582 HARPS FGK stars (Sousa+, 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/808/187 : Metallicities of KIC stars without planets (Buchhave+, 2015)
J/ApJS/220/19 : LAMOST obs. in the Kepler field. I. (De Cat+, 2015)
J/A+A/594/A39 : LAMOST-Kepler parameters & activity indicators (Frasca+, 2016)
J/AJ/151/144 : ASPCAP weights for 15 APOGEE chemical elements (Garcia+, 2016)
J/AJ/152/187 : Planet occurrence & stellar metallicity KOIs (Mulders+, 2016)
J/AJ/154/109 : California-Kepler Survey. III. Planet radii (Fulton+, 2017)
J/AJ/154/108 : California-Kepler Survey. II. Properties (Johnson+, 2017)
J/AJ/154/107 : California-Kepler Survey. I. 1305 stars (Petigura+, 2017)
J/ApJS/237/38 : Extended abundance analysis of KOIs (Brewer+, 2018)
J/ApJ/861/149 : Kepler Follow-up Obs. Program. II. Spectro. (Furlan+, 2018)
J/ApJ/860/109 : Keck HIRES obs. 245 subgiants (retired A tars) (Ghezzi+, 2018)
J/AJ/155/89 : California-Kepler Survey (CKS). IV. Planets (Petigura+, 2018)
J/ApJS/239/32 : APOKASC-2 catalog Kepler evolved stars (Pinsonneault+, 2018)
J/ApJS/235/38 : Kepler planetary cand VIII. DR25 reliability (Thompson+, 2018)
J/AJ/156/254 : CKS .VI. Kepler multis & singles (Weiss+, 2018)
J/AJ/155/68 : Elemental abundances of KOIs in APOGEE. I. (Wilson+, 2018)
J/ApJ/875/29 : Spectroscopic analysis of the CKS sample. I. (Martinez+, 2019)
J/ApJ/890/23 : NUV and FUV measurements of planet host stars (Loyd+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Star Stellar identifier
9- 16 F8.3 0.1nm Wave [5023/6862] Wavelength; Angstroms
18- 21 F4.1 --- Ion [26.0/26.1] Ion designation code (1)
23- 27 F5.3 eV ExPot [0.087/4.991] Excitation potential
29- 34 F6.3 [-] logg [-5.38/-0.22] log oscillator strength
36- 41 F6.3 [-] logG [-7.9/-7.09] log van der Waals damping constant at
1e4K (logΓw)
43- 47 F5.1 10-13m EW [5/191]? Equivalent width of Ion (2)
49- 52 F4.2 [-] Fe [6.6/8.6]? Iron abundance
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Note (1): Fe I and Fe II ions are represented by the notations 26.0 and 26.1,
respectively, following the format used by MOOG
Sneden, 1973PhDT.......180S 1973PhDT.......180S.
Note (2): Equivalent widths for some lines could not be measured by
ARES (Sousa+, 2015A&A...577A..67S 2015A&A...577A..67S) or were removed during the
iterative process (see Ghezzi+, 2018, J/ApJ/860/109 for more details).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Star Stellar identifier
9- 13 F5.2 [Sun] [Fe/H] [-0.57/0.45] Metallicity
15- 18 F4.2 [Sun] e_[Fe/H] [0.01/0.06] Uncertainty in [Fe/H]
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History:
From electronic version of the journal
References:
Martinez et al. Paper I : 2019ApJ...875...29M 2019ApJ...875...29M Cat. J/ApJ/875/29
(End) Prepared by [AAS], Coralie Fix [CDS], 06-Feb-2023