KEPLER 7.0 Astrology Software
Provides reliable and repeatable processing routines that remove instrumental artifacts from Kepler’s light curve data. This step is the key to the scientific analysis of the data, because any background sources, such as the blended spectrum of an eclipsing binary or zodiacal light, must first be removed. A number of processes are performed to determine whether a point in the light curve represents valid astrophysical data or instrumental artifacts. A total of ten potential artifacts are checked, including eclipses, transits, and period changes. The light curve parameters are checked for consistency, outliers and other potential problems are identified, and the data are checked for missing, erroneous, or as yet untypable data. The presence of all ten potential artifacts is marked in the light curve data file, and the artifact fields are cleaned before analysis. The accuracy of the data processing and the “cleaning” processes is monitored and improved as necessary.
Develops software algorithms based on the physics of Kepler’s orbit and internal hardware components to detect astrophysical transits and record the time of ingress and egress, and the duration of transit and eclipse. This process marks the start and end of Kepler’s photometric duty cycle.
…We will undertake a thorough and systematic analysis of the main science product of the mission, these light curves. This will involve a first pass of visual inspection, followed by detailed analysis of the data with the usual Kepler pipeline data reduction tools, and numerous custom scripts written in a variety of languages using a number of different techniques. From this analysis, we will identify candidate Kepler transiting planets, and perform a detailed followup on their characterisation via standard data reduction and analytical tools, as well as an expanded search for transit timing variations.
Study and identification of the light curve structures induced by exoplanet transits. Such transit structures can be used to infer the planetary radii and thus the planet-to-star size ratios from the apparent shape of the observed transits.
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