REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1–16 TRANSIT DETECTION RUN

By D. Huber, V. S. Aguirre, J. Matthews, M. Pinsonneault, E. Gaidos, Rafael A. Garc'ia, S. Hekker, S. Mathur, B. Mosser, G. Torres and 12 more. 2013

410 citations recorded by the source corpus.

We present revised properties for 196,468 stars observed by the NASA Kepler mission and used in the analysis of Quarter 1–16 (Q1–Q16) data to detect and characterize transiting planets. The catalog is based on a compilation of literature values for atmospheric properties (temperature, surface gravity, and metallicity) derived from different observational techniques (photometry, spectroscopy, asteroseismology, and exoplanet transits), which were then homogeneously fitted to a grid of Dartmouth stellar isochrones. We use broadband photometry and asteroseismology to characterize 11,532 Kepler targets which were previously unclassified in the Kepler Input Catalog (KIC). We report the detection of oscillations in 2762 of these targets, classifying them as giant stars and increasing the number of known oscillating giant stars observed by Kepler by ∼20% to a total of ∼15,500 stars. Typical uncertainties in derived radii and masses are ∼40% and ∼20%, respectively, for stars with photometric constraints only, and 5%–15% and ∼10% for stars based on spectroscopy and/or asteroseismology, although these uncertainties vary strongly with spectral type and luminosity class. A comparison with the Q1–Q12 catalog shows a systematic decrease in radii of M dwarfs, while radii for K dwarfs decrease or increase depending on the Q1–Q12 provenance (KIC or Yonsei–Yale isochrones). Radii of F–G dwarfs are on average unchanged, with the exception of newly identified giants. The Q1–Q16 star properties catalog is a first step toward an improved characterization of all Kepler targets to support planet-occurrence studies.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Charbonneau
2. Timothy Morton
3. D. Huber
4. J. Johnson
5. E. Gaidos
6. Jon Fortney
7. J. Winn
8. G. Marcy

In Computational Mechanics

1. D. Huber
2. Jon M. Jenkins
3. D. Charbonneau
4. D. Stello
5. Y. Elsworth
6. T. Bedding
7. S. Hekker
8. T. Kallinger

In Instrumentation

1. D. Charbonneau
2. Timothy Morton
3. D. Huber
4. E. Gaidos
5. J. Winn
6. J. Johnson
7. C. Dressing
8. E. Petigura

Citations in the corpus

• STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION (2015, neutral): “We note the observed photometric parameters are consistent with spectroscopically derived parameters for stars with published spectra, and consistent with typical model-dependent uncertainties from photometric data (e.g., Huber et al. 2014).”
• REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, background): “We collected stars with spectroscopically or asteroseismically determined stellar properties from Huber et al. (2014), but excluded stars from Buchhave et al. (2012).”
• The California-Kepler Survey. VII. Precise Planet Radii Leveraging Gaia DR2 Reveal the Stellar Mass Dependence of the Planet Radius Gap (2018, background): “Until recently, the properties of the vast majority of Kepler planet host stars were based on photometry alone, i.e., from the Kepler Input Catalog (KIC) and its updates (Brown et al. 2011; Huber et al. 2014; Mathur et al. 2017).”
• PLANETARY CANDIDATES OBSERVED BY KEPLER. VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS) (2015, background): “Huber et al. (2014) describe the latest results of an ongoing effort to construct an internally consistent catalog of stellar radius drawing from photometry, spectroscopy and asteroseismology.”
• AN EMPIRICAL CALIBRATION TO ESTIMATE COOL DWARF FUNDAMENTAL PARAMETERS FROM H-BAND SPECTRA (2014, methodology): “We calculate Teq using either our new stellar effective temperature or that from Huber et al. (2014).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, methodology): “Our sample has been extracted from the 77 exoplanet host stars presented in Huber et al. (2013b).”
• TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, methodology): “In this study, we adopt stellar parameters from the Q1-Q16 KIC revision of Huber et al. (2014).”
• Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, methodology): “The SAGA asteroseismic catalogue consists of 989 stars identified by cross-matching our Strömgren observations with the dwarf sample of Chaplin et al. (2014) and the 15 000 giants from the Kepler Asteroseismic Science Consortium (KASC; Stello et al. 2013; Huber et al. 2014).”
• Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes (2016, background): “…of the star, glog (which is a direct observable from high-resolution spectra), astroseismological inferences of the stellar mass and radius (e.g., Huber et al. 2013), or a measurement of the radius of the star (which, as we will show is a direct observable from the bolometric flux and effective…”
• THE KEPLER FOLLOW-UP OBSERVATION PROGRAM. I. A CATALOG OF COMPANIONS TO KEPLER STARS FROM HIGH-RESOLUTION IMAGING (2016, methodology): “We also assumed that Kp magnitudes correspond to R magnitudes, and we adopted effective temperatures (Teff ) for the primary stars from the stellar parameters of Huber et al. (2014).”
• The Gaia–Kepler Stellar Properties Catalog. I. Homogeneous Fundamental Properties for 186,301 Kepler Stars (2020, methodology): “Due to the long baseline, high precision observations and subsequent follow-up efforts, the Kepler target stars have become one of the best-characterized samples of stars (Huber et al. 2014; Mathur et al. 2017; Berger et al. 2018b).”
• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, background): “…time-domain variability of stars offers currently the highest precision log g values for field stars, for example by measuring amplitudes or timescales of stellar granulation (≈ 0.1 dex, Bastien et al. 2013; ≈ 0.03 dex, Kallinger et al. 2016) or stellar oscillations (≈ 0.01 dex, Huber et al. 2013).”
• HOW ROCKY ARE THEY? THE COMPOSITION DISTRIBUTION OF KEPLER’S SUB-NEPTUNE PLANET CANDIDATES WITHIN 0.15 AU (2014, methodology): “Matching Q1-12 PCs to Q1-16 TCEs also ensures that the planet parameters used in our analysis are those derived with the best-knowledge stellar parameters: the Q1-16 stellar properties are described in Huber et al. (2014), hereafter referred to as Hub14.”
• THE K2 ECLIPTIC PLANE INPUT CATALOG (EPIC) AND STELLAR CLASSIFICATIONS OF 138,600 TARGETS IN CAMPAIGNS 1–8 (2015, background): “Since the majority of stars with log g ≈ 2 − 3.4 and Kp < 15 should show detectable oscillations with K2 (Stello et al. 2015), asteroseismic analyses are also efficient to discern luminosity classes of Kepler and K2 targets (Huber et al. 2013).”