Polaroid ST-8E, ST-9E, ST-7E manual Double Correlated Sampling Readout, Dark Frames

Page 13

Section 2 - Introduction to CCD Cameras

have a single stage TE cooler and a temperature sensing thermistor on the CCD mount to monitor the temperature. The ST-9E has a supplemental second stage cooling booster with water cooling as an option (described in section 6.1). The microcontroller controls the temperature at a user-determined value for long periods. As a result, exposures hours long are possible, and saturation of the CCD by the sky background typically limits the exposure time. The temperature regulation feature of the ST-7E, ST-8E and ST-9E also means that one dark frame can be used for similar exposures on several nights. At 0 °C the dark current in the ST- 7E and ST-8E, high-resolution mode, is only 36 electrons per minute! The ST-9E, with it's bigger pixels, has roughly 15 times this amount of dark current, 5 times due to the larger pixel area and 3 times due to the inherent higher bulk dark current in the device. That's why we include the cooling booster with the ST-9E.

The sky background conditions also increase the noise in images, and in fact, as far as the CCD is concerned, there is no difference between the noise caused by dark current and that from sky background. If your sky conditions are causing photoelectrons to be generated at the rate of 100 e-/pixel/sec, for example, increasing the cooling beyond the point where the dark current is roughly half that amount will not improve the quality of the image. This very reason is why deep sky filters are so popular with astrophotography. They reduce the sky background level, increasing the contrast of dim objects. They will improve CCD images from very light polluted sights.

2.4.2. Double Correlated Sampling Readout

During readout, the charge stored in a pixel is stored temporarily on a capacitor. This capacitor converts the optically generated charge to a voltage level for the output amplifier to sense. When the readout process for the previous pixel is completed, the capacitor is drained and the next charge shifted, read, and so on. However, each time the capacitor is drained, some residual charge remains.

This residual charge is actually the dominant noise source in CCD readout electronics. This residual charge may be measured before the next charge is shifted in, and the actual difference calculated. This is called double correlated sampling. It produces more accurate data at the expense of slightly longer read out times (two measurements are made instead of one). The ST-7E, ST-8E and ST-9E utilize double correlated sampling to produce the lowest possible readout noise. At 13e- to 15e- rms per read these cameras are unsurpassed in performance.

2.4.3. Dark Frames

No matter how much care is taken to reduce all sources of unwanted noise, some will remain. Fortunately, however, due to the nature of electronic imaging and the use of computers for storing and manipulating data, this remaining noise can be drastically reduced by the subtraction of a dark frame from the raw light image. A dark frame is simply an image taken at the same temperature and for the same duration as the light frame with the source of light to the CCD blocked so that you get a "picture" of the dark. This dark frame will contain an image of the noise caused by dark current (thermal noise) and other fixed pattern noise such as read out noise. When the dark frame is subtracted from the light frame, this pattern noise is removed from the resulting image. The improvement is dramatic for exposures of more than a

Page 9

Page 12 Page 14
Image 13
Page 12 Page 14
Contents Operating Manual Page Table of Contents Technique Road Map of the Documentation IntroductionQuick Tour Ccdops for Windows or Macintosh Ccdops SoftwareCCD Camera Page Cameras in General Introduction to CCD CamerasHow CCD Detectors Work Camera Hardware Architecture Full Frame and Frame Transfer CCDsCCD System Block Diagram Cooling CCD Special RequirementsDark Frames Double Correlated Sampling ReadoutPixels vs. Film Grains Flat Field ImagesGuiding Electronic Imaging Black and White vs. Color Page Step by Step with a CCD Camera At the Telescope with a CCD CameraAttaching the Camera to the Telescope Establishing a Communications Link Focusing the CCD CameraCamera Back Focus Taking an Image Finding and Centering the ObjectDisplaying the Image Processing the ImageAdvanced Capabilities Crosshairs Mode Photometry and AstrometrySub-Frame Readout in Focus Autoguiding and Self Guiding Track and AccumulateColor Imaging Auto GrabAt the Telescope with a CCD Camera Connecting to the Computer Connecting the PowerConnecting the Relay Port to the Telescope Camera HardwareUsing Mechanical Relays Push to Make Switch Modification Joystick Modification Modular Family of CCD CamerasSystem Features 20.6x sizeum Focal length cm Camera Hardware Connecting the older model CFW-6 filter wheel to the Camera Battery Operation Page Lunar and Planetary Imaging Advanced Imaging TechniquesDeep Sky Imaging Terrestrial ImagingTaking a Good Flat Field Changing the Camera ResolutionBuilding a Library of Dark Frames Flat Fielding Track and Accumulate Images Tracking Functions Advanced Imaging Techniques Page Cooling Booster Accessories for your CCD CameraCamera Lens Adapters and Eyepiece Projection Tri-color ImagingFocal Reducers AO-7 and Lucy-Richardson SoftwareSGS Self-Guided Spectrograph Third Party Products and ServicesWindows Software Image Processing SoftwareSbig Technical Support Common Problems Common Problems Common Problems Page Glossary STV Glossary Glossary Appendix a Connector Pinouts Appendix a Connector ad CablesSbig Tracking Interface Cable TIC-78 Figure A1 CCD Connector for TIC Mating Cleaning the CCD and the Window Appendix C MaintenanceRegenerating the Desiccant Page Technique Appendix C Capturing a Good Flat FieldPage Index IBM PC Separations
Top Page Image Contents