Transiting planet search in the Kepler pipeline

By Jon M. Jenkins, H. Chandrasekaran, S. McCauliff, Douglas A. Caldwell, P. Tenenbaum, Jie Li, T. Klaus, M. Cote, C. Middour. Astronomical Telescopes + Instrumentation, 2010

174 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Signal Processing

View Paper: https://www.semanticscholar.org/paper/2ab8dab6d23849de88182d7ba5a31050a81bffee

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Citations in the corpus

The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets (2017, methodology): “They injected about ten-thousand transit signals into the raw pixel data and processed the results with version 9.1 of the official Kepler pipeline (Jenkins et al. 2010).”
AUTOMATIC CLASSIFICATION OF KEPLER PLANETARY TRANSIT CANDIDATES (2014, methodology): “MESmin is the minimum MES discovered by the TPS, indicating repeated events above the baseline stellar flux.”
THE FALSE POSITIVE RATE OF KEPLER AND THE OCCURRENCE OF PLANETS (2013, methodology): “(1) In this expression erf is the standard error function, and the adopted 7.1σ threshold was chosen so that no more than one false positive will occur over the course of the Mission due to random fluctuations (see Jenkins et al. 2010).”
CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BY KEPLER. II. ANALYSIS OF THE FIRST FOUR MONTHS OF DATA (2011, methodology): “Steps such as high-precision RV measurements (Borucki et al. 2010; Koch et al. 2010b; Dunham et al. 2010; Jenkins et al. 2010a; Latham et al. 2010) or transit timing variations (TTVs; Holman et al. 2010; Lissauer et al. 2011a) are used when practical.”
The TESS science processing operations center (2016, methodology): “The metric used for both the TESS and Kepler missions is the combined differential photometric precision (CDPP).(7)”
KEPLER'S FIRST ROCKY PLANET: KEPLER-10b (2011, methodology): “Data for up to 170,000 stars are recorded at LC, while data for up to 512 stars are also co-added to a 58.85 s (∼1 minute) integration (9 readouts) termed short cadence (SC) as described in Jenkins et al. (2010b) and Gilliland et al. (2010).”
The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets (2017, methodology): “…et al. 2011; Bryson et al. 2010; Haas et al. 2010), as well as the software engineering that transformed CCD pixel values into planet candidates (Jenkins et al. 2010; Gilliland et al. 2010; Stumpe et al. 2012; Smith et al. 2012, 2016; Batalha et al. 2010a,b; Torres et al. 2011; Bryson et al.…”
DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R⨁ SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR (2015, methodology): “To search for transit signatures, TPS employs a bank of wavelet-based matched filters that form a grid on a three-dimensional parameter space of transit duration, orbital period, and phase (Jenkins 2002; Jenkins et al. 2010).”
PLANETARY CANDIDATES OBSERVED BY KEPLER. III. ANALYSIS OF THE FIRST 16 MONTHS OF DATA (2012, methodology): “Fourteen distinct transit searches are conducted, each using a different pulse duration (1.5, 2.0, 2.5, 3.0, 3.5, 4.5, 5.0, 6.0, 7.5, 9.0, 10.5, 12.0, 12.5, and 15 hr) as described in Jenkins et al. (2010b) and Tenenbaum et al. (2012).”
Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90 (2017, methodology): “…from lists of “threshold crossing events” (TCEs; detected periodic signals that may be consistent with transiting planets) from the Kepler pipeline (Jenkins et al. 2010b,c), which were manually culled by humans to remove false positives caused by astrophysical variability and instrumental…”
TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26 (2021, methodology): “The SPOC pipeline also searches the PDC light curves for transiting planet signatures using an adaptive, wavelet-based matched filter (Jenkins 2002; Jenkins et al. 2010), and the resulting TCEs are fitted with an initial limb-darkened transit model (Li et al. 2019) and subjected to a suite of…”
A PLATEAU IN THE PLANET POPULATION BELOW TWICE THE SIZE OF EARTH (2013, methodology): “(1) Our approach is similar to the widely-used BLS algorithm of Kovács et al. (2002) as well as to the TPS component of the Kepler pipeline (Jenkins et al. 2010b).”
CHARACTERISTICS OF KEPLER PLANETARY CANDIDATES BASED ON THE FIRST DATA SET (2010, methodology): “6 Jupiter radii and orbital periods from 3.2 to 4.9 days were confirmed by radial velocity observations (Borucki et al. 2010, Koch et al. 2010a, Dunham et al. 2010, Jenkins et al. 2010a, and Latham et al. 2010).”
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): “The data from the spacecraft are processed through the Kepler Science Operations Center pipeline (Jenkins et al. 2010c) to perform standard CCD processing and to remove instrumental artifacts.”
HOW ROCKY ARE THEY? THE COMPOSITION DISTRIBUTION OF KEPLER’S SUB-NEPTUNE PLANET CANDIDATES WITHIN 0.15 AU (2014, methodology): “The automated portion of this process is the pipeline developed by the Kepler Mission Science Operations Center (SOC), as outlined in Jenkins et al. (2010); it includes modules that calibrate the raw images from the Kepler spacecraft (Quintana et al. 2010), produce raw photometry from these images…”
Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs (2019, methodology): “The 2 minute cadence data were extracted using the Science Processing Operations Center (SPOC) pipeline, a descendant of the Kepler mission pipeline (Jenkins 2002; Jenkins et al. 2010, 2016; Jenkins 2017; Stumpe et al. 2014; Smith et al. 2012).”