Some Tests to Establish Confidence in Planets Discovered by Transit Photometry

By Jon M. Jenkins, Douglas A. Caldwell, William J. Borucki. 2002

149 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/015f18097688d2e0ddcf0485ef05434ca10436c7

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Citations in the corpus

Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, methodology): “Errorbars are also calculated using a residual permutation(or “prayer bead”) algorithm (Jenkins et al. 2002) which accounts for correlated observational noise, and the largest of the two altern - tives is adopted for each parameter.”
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…”
THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES (2015, methodology): “The choice of an appropriate SNR threshold was discussed in detail by Jenkins et al. (2002) in the context of the Kepler mission.”
The Impact of Solar-like Variability on the Detectability of Transiting Terrestrial Planets (2002, methodology): “Moreover, 50% of transits are longer than 11.3 hr.) The total number of effective independent tests to be performed in searching the light curves of 100,000 stars for transiting planets with orbital periods in this range is 2 1012 (Jenkins et al. 2002).”
The Derivation, Properties, and Value of Kepler’s Combined Differential Photometric Precision (2012, background): “We define a threshold crossing event as a signal which, when folded at a given period, gives rise to a signal of ≥7:1σ (Jenkins et al. 2002).”
VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. II. REFINED STATISTICAL FRAMEWORK AND DESCRIPTIONS OF SYSTEMS OF SPECIAL INTEREST (2014, background): “Stochastic noise is expected to produce no more than one spurious transiting planet signature with S/N > 7.1 over Kepler’s entire four year mission (Jenkins et al. 2002).”
PLANETARY CANDIDATES OBSERVED BY KEPLER. VI. PLANET SAMPLE FROM Q1–Q16 (47 MONTHS) (2015, background): “MES is defined in detail in Jenkins et al. (2002), but is equivalent to the signal-to-noise ratio of the transit detection in the folded lightcurve.”
DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R⨁ SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR (2015, methodology): “Jenkins et al. (2002) formulated a bootstrap test for establishing the confidence level in plan- etary transit signatures identified in transit photometry in white, but possibly non-Gaussian noise.”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, methodology): “I therefore also runa residual permutation (or “prayer bead”) algorithm (Jenkins et al. 2002) with the quadratic LD law.”
Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90 (2017, methodology): “…higher S/NBLS thresholds are used for two reasons: a) to prevent the number of spurious TCEs (caused by systematics or otherwise) from overwhelming the number of real detected planets, and b) to ensure that no TCEs produced by purely Gaussian fluctuations are detected (e.g. Jenkins et al. 2002).”
Homogeneous studies of transiting extrasolar planets – I. Light-curve analyses (2008, methodology): “…of how red noise affects the analysis of TEPs is given by Pont et al. (2006) To assess the effect of systematic errors on the uncertainties of the light curve parameter measurements, I have implemented into jktebop a residual-permutation (or “prayer bead”) algorithm (Jenkins et al. 2002).”
The WASP Project and the SuperWASP Cameras (2006, background): “For example, the Vulcan project (Jenkins et al. 2002) searched some 6000 stars, finding only seven transit-like variables.”
TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, background): “…the pipeline completeness (fraction of transit signals present in the data that are recovered by the pipeline) has a theoretical expected form of Pdet(MES) = 1 2 + 1 2 erf [ (MES−MESthresh)√ 2 ] , (4) where MESthresh = 7.1 is the adopted detection threshold (Jenkins et al. 2002; Jenkins 2002).”
High-precision photometry by telescope defocussing. I. The transiting planetary system WASP-5 (2009, methodology): “This does not account for any systematic errors which might be in our light curves, so this possibility was investigated using the residualpermutation approach (Jenkins et al. 2002) and found to be marginally significant.”