The Impact of Solar-like Variability on the Detectability of Transiting Terrestrial Planets

By Jon M. Jenkins. 2002

228 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/767d51e703e0883e1581551e6de7848a235b595f

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Citations in the corpus

PLANETARY CANDIDATES OBSERVED BY KEPLER. III. ANALYSIS OF THE FIRST 16 MONTHS OF DATA (2012, methodology): “The TPS pipeline algorithm measures σcdpp over a grid of transit durations from 1.5 to 15.0 hr (Jenkins 2002; Christiansen et al. 2012), and we interpolate to determine the photometric noise at the estimated duration expected.”
KEPLER MISSION DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE (2010, background): “Analysis of data from the Sun shows that variability during solar maximum on the timescale of a transit is typically 10 ppm (Jenkins 2002).”
OVERVIEW OF THE KEPLER SCIENCE PROCESSING PIPELINE (2010, methodology): “TPS searches for transiting planets by ”stitching” the quarterly segments of data together to remove gaps and edge effects and then applies the wavelet-based, adaptive matched filter of Jenkins (2002).”
KEPLER ECLIPSING BINARY STARS. VII. THE CATALOG OF ECLIPSING BINARIES FOUND IN THE ENTIRE KEPLER DATA SET (2015, background): “All transit events were identified by the main Kepler pipeline (Jenkins 2002; Jenkins et al. 2010) and through the following sources explained here.”
PLANETARY CANDIDATES OBSERVED BY KEPLER IV: PLANET SAMPLE FROM Q1–Q8 (22 MONTHS) (2013, methodology): “TPS empirically determines the noise in the flux time series (combined differential photometric precision, CDPP, Christiansen et al. 2012) of each target to search for potential planet candidates (threshold crossing events, TCEs) (Jenkins 2002; Tenenbaum et al. 2012).”
KEPLER ECLIPSING BINARY STARS. II. 2165 ECLIPSING BINARIES IN THE SECOND DATA RELEASE (2011, background): “As periods up to the length of the data are considered, strong single transits or eclipses are detected as well as series of transits (Jenkins 2002, Eq.”
The Derivation, Properties, and Value of Kepler’s Combined Differential Photometric Precision (2012, background): “The theoretical basis of the approach is described in Jenkins (2002).”
CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BY KEPLER. II. ANALYSIS OF THE FIRST FOUR MONTHS OF DATA (2011, methodology): “…a wavelet-based, adaptive matched filter that characterizes the power spectral density (PSD) of the background process yielding the observed light curve and uses this time-variable PSD estimate to realize a pre-whitening filter and whiten the light curve (Jenkins 2002; Jenkins et al. 2010c, 2010d).”
AUTOMATIC CLASSIFICATION OF KEPLER PLANETARY TRANSIT CANDIDATES (2014, methodology): “The TPS algorithm detects transit-like features in light curves by applying a noise-compensating, wavelet-based matched filter (Jenkins 2002).”
Analytic Light Curves for Planetary Transit Searches (2002, methodology): “This code will be useful for simulating planetary transit searches (Gaudi2000; Defaÿ et al. 2001; Jenkins et al. 2002; Remund et al. 2002; Jenkins 2002; Pepper & Gould 2002), searching for planetary transit signals in lightcurves collected by a given search,and for fitting and measuring the errors…”
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).”
KEPLER ECLIPSING BINARY STARS. I. CATALOG AND PRINCIPAL CHARACTERIZATION OF 1879 ECLIPSING BINARIES IN THE FIRST DATA RELEASE (2010, methodology): “…is a wavelet-based, adaptive matched filter that characterizes the power spectral density (PSD) of the background process that yields the observed light curve and uses this time-variable PSD estimate to realize a pre-whitening filter and whiten the light curve (Jenkins 2002; Jenkins et al. 2010d).”
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).”
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…”
TRANSIT DETECTION IN THE MEarth SURVEY OF NEARBY M DWARFS: BRIDGING THE CLEAN-FIRST, SEARCH-LATER DIVIDE (2012, methodology): “To identify candidate transiting planets and assess their significance, Kepler employs a waveletbased matched filter that is both optimal and efficient (Jenkins 2002; Tenenbaum et al. 2012).”
The TESS Objects of Interest Catalog from the TESS Prime Mission (2021, methodology): “…the power spectral density of the observation noise, then estimating the likelihood of a transit over a range of trial transit durations and orbital periods as a function of time over the observations, quantified as the single-event statistic (SES; Jenkins 2002, 2020; Jenkins et al. 2010).”