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This paper summarizes the introductory presentation for a workshop thatexplored the challenges of making precision astronomical measurements usingdeeply depleted (thick) CCDs. While thick CCDs provide definite advantages interms of increased quantum efficiency at NIR wavelengths, and reduced fringingfrom atmospheric emission lines, these devices also exhibit undesirablefeatures that pose a challenge to precision determination of the positions,fluxes, and shapes of astronomical objects, and features in astronomicalspectra. Many of the effects seen in these devices arise from lateralelectrical fields within the detector, that produce charge transport anomaliesthat have been previously misinterpreted as quantum efficiency variations.Performing simplistic flat-fielding introduces systematic errors in the imageprocessing pipeline. One measurement challenge is devising a calibration methodthat can distinguish genuine quantum efficiency variations from chargetransport effects. Given the scientific benefits of improving both theprecision and accuracy of astronomical measurements, we need to identify,characterize, and overcome these various detector artifacts. In retrospect,many of the detector features first identified in thick CCDs also afflictmeasurements made with more traditional CCD detectors, albeit often at areduced level. I provide a qualitative overview of the physical effects wethink are responsible for the observed device properties, and provide someperspective for the work that lies ahead. Finally, I take this opportunity tomake a plea for establishing a clear and consistent vocabulary when describingthese various detector features, and make some suggestions for a standardlexicon based on discussions at the workshop.

Precision Astronomy with Imperfect Fully Depleted CCDs -- An Introduction and a Suggested Lexicon