The Kepler telescope uses a Charge-Coupled Detector (CCD) to measure the brightness of distant stars and looks for the transits of exoplanets passing in front of their host stars. The Kepler mission currently uses a Pixel Response Function (PRF) which is modeled and empirically derived to analyze the distribution of light from a given star. This PRF can be drastically improved by taking measured data in a controlled environment to map it out, which we will do with wavelengths across the visible spectrum. We will direct a spot of light across the area of each pixel, measuring differences in intensity so that we can create an Intrapixel Response Function (IPRF) for each wavelength. This IPRF will allow us to better understand previous and current data from the Kepler missions.
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