J/AJ/159/281 Characteristics of 335 KOI stars (Gilbert+, 2020)
An information theoretic framework for classifying exoplanetary system
architectures.
Gilbert G.J., Fabrycky D.C.
<Astron. J., 159, 281 (2020)>
=2020AJ....159..281G 2020AJ....159..281G
ADC_Keywords: Stars, variable; Stars, masses; Exoplanets; Optical
Keywords: Exoplanet systems ; Astroinformatics ; Classification systems
Abstract:
We propose several descriptive measures to characterize the
arrangements of planetary masses, periods, and mutual inclinations
within exoplanetary systems. These measures are based on complexity
theory and capture the global, system-level trends of each
architecture. Our approach considers all planets in a system
simultaneously, facilitating both intrasystem and intersystem
analysis. We find that based on these measures, Kepler's
high-multiplicity (N≥3) systems can be explained if most
systems belong to a single intrinsic population, with a subset of
high-multiplicity systems (∼20%) hosting additional, undetected
planets intermediate in period between the known planets. We confirm
prior findings that planets within a system tend to be roughly the
same size and approximately coplanar. We find that forward modeling
has not yet reproduced the high degree of spacing similarity (in log-
period) actually seen in the Kepler data. Although our classification
scheme was developed using compact Kepler multis as a test sample, our
methods can be immediately applied to any other population of
exoplanetary systems. We apply this classification scheme to
1- quantify the similarity between systems,
2- resolve observational biases from physical trends,
3- identify which systems to search for additional planets and where
to look for these planets.
Description:
When evaluating these measures on real systems, we use the catalog
from the California Kepler Survey (CKS). To ensure a high-quality
sample, we cross-match all candidate planets with Kepler Data Release
25 (DR25). All of the stars in the sample have been well characterized
by Gaia DR1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 49 335 Summary of system-level measures
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
J/MNRAS/410/166 : Morphological types from Galaxy Zoo 1 (Lintott+, 2011)
J/ApJS/197/8 : Kepler's cand. multiple transiting planets (Lissauer+, 2011)
J/ApJ/763/41 : Kepler multiple-candidate systems radii (Ciardi+, 2013)
J/MNRAS/435/2835 : Morphological types from Galaxy Zoo 2 (Willett+, 2013)
J/ApJ/790/146 : Planets Kepler's multi-transiting systems (Fabrycky+, 2014)
J/MNRAS/448/3608 : Titius-Bode-based exoplanet predictions (Bovaird+, 2015)
J/ApJ/825/19 : Mass-radius relation for planets with Rp<4 (Wolfgang+, 2016)
J/ApJ/834/17 : Mass & radius of planets, moons, low mass stars (Chen+,2017)
J/AJ/153/71 : Kepler follow-up obs. program. I. Imaging (Furlan+, 2017)
J/AJ/154/108 : California-Kepler Survey. II. Properties (Johnson+, 2017)
J/A+A/605/A72 : Planetary systems AMD-stability (Laskar+, 2017)
J/AJ/154/107 : California-Kepler Survey. I. 1305 stars (Petigura+, 2017)
J/AJ/156/264 : California-Kepler Survey. VII. Planet radius (Fulton+, 2018)
J/AJ/155/205 : Occurrence rates Q1-Q16 KOI catalog planet cand. (Hsu+,2018)
J/ApJS/235/38 : Kepler planet cand. VIII. DR25 reliability (Thompson+, 2018)
J/AJ/155/48 : California-Kepler Survey. V. Masses & radii (Weiss+, 2018)
J/AJ/158/109 : Occurrence rates of planets orbiting FGK stars (Hsu+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- KOI Kepler Object of Interest (KOI) number (1)
11- 16 F6.3 [-] logMdyn [-5.86/-3.12] Log dynamical mass (log10µ)
18- 22 F5.3 --- Q [0/0.98] Mass partitioning
24- 28 F5.2 --- M [-0.92/0.99] Monotonicity
30- 33 F4.1 --- S [3.9/91.4] Characteristic spacing
35- 39 F5.3 --- C [0/0.94]? Gap complexity
41- 45 F5.3 --- f [0/0.64] Flatness
47 I1 --- N [2/7] Multiplicity
49 A1 --- pop ?=- Population assignment via clustering (2)
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Note (1): Some variables are undefined for systems with N<3, but
systems with N=2 are included for completeness.
Note (2): Assignements as follows:
0 = Larger primary cluster centers around low Q, C, and f, with S∼20
(102 occurrences).
1 = Smaller secondary cluster extends out to high values of C, S
(27 occurrences).
Details about clustering can be found in sections 4 and 6 of the article.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 31-Aug-2020