SELECTION, PRIORITIZATION, AND CHARACTERISTICS OF KEPLER TARGET STARS

By N. Batalha, William J. Borucki, D. Koch, S. Bryson, M. Haas, T. Brown, Douglas A. Caldwell, J. Hall, R. Gilliland, D. Latham and 2 more. 2010

226 citations recorded by the source corpus.

The Kepler Mission began its 3.5 year photometric monitoring campaign in 2009 May on a select group of approximately 150,000 stars. The stars were chosen from the ∼ half million in the field of view that are brighter than 16th magnitude. The selection criteria are quantitative metrics designed to optimize the scientific yield of the mission with regard to the detection of Earth-size planets in the habitable zone. This yields more than 90,000 G-type stars on or close to the main sequence, >20, 000 of which are brighter than 14th magnitude. At the temperature extremes, the sample includes approximately 3000 M-type dwarfs and a small sample of O- and B-type MS stars (<200). The small numbers of giants are included in the sample: ∼5000 stars with surface gravities log(g) < 3.5. We present a brief summary of the selection process and the stellar populations it yields in terms of surface gravity, effective temperature, and apparent magnitude. In addition to the primary, statistically derived target set, several ancillary target lists were manually generated to enhance the science of the mission, examples being: known eclipsing binaries, open cluster members, and high proper motion stars.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ff0fb8e7aefaa9a8c9a29e9801ddd75d69b4c541

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Citations in the corpus

• PHOTOMETRIC VARIABILITY IN KEPLER TARGET STARS. II. AN OVERVIEW OF AMPLITUDE, PERIODICITY, AND ROTATION IN FIRST QUARTER DATA (2010, methodology): “There are features in the log(g)-Teff plane that are due to artifacts in the way the KIC was constructed and in target selection criteria for the exoplanet search (Batalha et al. 2010).”
• Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, background): “The selection criteria of the satellite were designed to optimize the scientific yield of the mission with regard to the detection of Earth-size planets in the habitable zone of cool main-sequence stars (Batalha et al. 2010).”
• THE OCCURRENCE RATE OF SMALL PLANETS AROUND SMALL STARS (2013, unknown): “…al. (2012) also improved the stellar parameters for many target stars by comparing the estimated temperatures, radii, and surface gravities in the Kepler Input Catalog (KIC; Batalha et al. 2010; Brown et al. 2011) to the values expected from Yonsei-Yale evolutionary models (Demarque et al. 2004).”
• Kepler-22b: A 2.4 EARTH-RADIUS PLANET IN THE HABITABLE ZONE OF A SUN-LIKE STAR (2011, background): “The statistical properties of stars targeted by Kepler are described by Batalha et al. (2010a).”
• The first data release (DR1) of the LAMOST regular survey (2015, background): “…targets (∼250, MK secondary standard stars), KASC targets (∼7000, selected by theKeplerAsteroseismic Science Consortium, or KASC), planet targets (∼150 000, selected by the Keplerplanet search group, Batalha et al. 2010), and extra targets(∼1 000 000 other targets in the KeplerFoV from the KIC 10).”
• OVERVIEW OF THE KEPLER SCIENCE PROCESSING PIPELINE (2010, background): “If so, the source right ascension and declination can be estimated by the measured in- versus out-of-transit centroid shift normalized by the fractional change in brightness of the system (i.e., the transit ”depth”; Batalha et al. 2010b; Monet et al. 2010).”
• The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets (2017, background): “Targets fainter than Kp > 14.0 were observed by Kepler only if their stellar and noise properties indicated that there was a high probability of the detection of small planets (Batalha et al. 2010).”
• KEPLER MISSION DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE (2010, methodology): “…fit and remove local background for each star (Jenkins et al. 2010a), (6) measure any centroid shift during a transit at the sub-millipixel level (Batalha et al. 2010a), (7) perform astrometry and obtain parallaxes and hence distances to the stars (Monet et al. 2010), and (8) reprocess the data…”
• KEPLER'S FIRST ROCKY PLANET: KEPLER-10b (2011, methodology): “Data validation for Kepler’s first planet discoveries (Kepler-4b, 5b, 6b, 7b, and 8b) is described in Batalha et al. (2010b).”
• KEPLER-18b, c, AND d: A SYSTEM OF THREE PLANETS CONFIRMED BY TRANSIT TIMING VARIATIONS, LIGHT CURVE VALIDATION, WARM-SPITZER PHOTOMETRY, AND RADIAL VELOCITY MEASUREMENTS (2011, methodology): “Batalha et al. (2010b) discuss the selection and characteristics of the Kepler target stars.”
• SPECTRO-THERMOMETRY OF M DWARFS AND THEIR CANDIDATE PLANETS: TOO HOT, TOO COOL, OR JUST RIGHT? (2013, background): “Although Kepler target stars are mostly F, G, and early K dwarfs (Batalha et al. 2010), there are also ∼4000 Kepler stars cooler than 4000 K (Dressing & Charbonneau 2013), which collectively harbor more than 100 detected candidate exoplanets.”
• LARGER PLANET RADII INFERRED FROM STELLAR “FLICKER” BRIGHTNESS VARIATIONS OF BRIGHT PLANET-HOST STARS (2014, methodology): “For stars with 6500 K>Teff>4700 K and Kepmag<13, the Kepler target sample should be representative of the field for all but evolved giants with log g<3.5 (Batalha et al. 2010).”
• KEPLER ECLIPSING BINARY STARS. VII. THE CATALOG OF ECLIPSING BINARIES FOUND IN THE ENTIRE KEPLER DATA SET (2015, background): “The details and characteristics of the Kepler instrument and observing program can be found in Batalha et al. (2010), Borucki et al. (2011), Caldwell et al. (2010), Koch et al. (2010).”
• THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “The Kepler target list (Batalha et al. 2010) consists of 2×105 stars which are optically bright (Kp 16) and comprises 105 G dwarfs (explicitly selected to be suitable for detecting Earth analogs), 2×104 F dwarfs, 2×104 K dwarfs, 3×103 M dwarfs, 103 OBA dwarfs, and at least 1.5×104 giants of all…”
• KEPLER MISSION STELLAR AND INSTRUMENT NOISE PROPERTIES (2011, background): “Since red giants are inherently much noisier than dwarfs, and many of these have been dropped (Batalha et al. 2010) from the planetary target list, we replicated the observed red giants to bring their total fraction up to 50%.”