CCDs have revolutionized astronomical imaging. With earlier photographic plate technology one had a different detector for every exposure. Because the same CCD detector is used for all exposures, it is possible to correct for its defects with one set of calibrations. By combining many of these corrected CCD exposures it is then possible to image far fainter objects. Another CCD advantage is its huge dynamic range in the stored image: from ten electrons to as much as 200,000 electrons per pixel.

Experiment Guides

  • Pre Lab
  • Observing Guide
  • Operations
  • Python Image Reduction Handbook
  • 9.65 AB mag Calibration Star
  • Backup calibration method
  • Related Material

  • Chromey (2010) Chapter 3
  • Observing Data and Info
  • KAF-1001E CCD datasheet
  • Apogee U6 Timing Diagram
  • Apogee U6 Information
  • Filter Transmission Curves
  • Useful Links

  • JskyCalc Observing Aid
  • Intro ray optics
  • Parabola via Fermat!