Difference between revisions of "Flat-field correction"
(→Correcting an image) |
|||
| Line 9: | Line 9: | ||
==Correcting an image== | ==Correcting an image== | ||
[[File:Flat-field correction.png|thumb|right|The effect of nonuniform illumination and camera response can be reduced by flat-field correction, which involves dividing the non-uniformly illuminated image by a reference image that maps the illumination intensity. The black level must be subtracted from image to be corrected and the reference image in order to apply the proper correction.]] | [[File:Flat-field correction.png|thumb|right|The effect of nonuniform illumination and camera response can be reduced by flat-field correction, which involves dividing the non-uniformly illuminated image by a reference image that maps the illumination intensity. The black level must be subtracted from image to be corrected and the reference image in order to apply the proper correction.]] | ||
| + | The value of each pixel in the image is equal to <math>P_i = R_i I_i + D_i</math>, where <math>P_i</math> is the pixel value recorded by the camera for the ''i''th pixel; <math>R_i</math> is the responsivity of the ''i''th pixel; <math>I_i</math> is the intensity of light incident on the ''i''th pixel; and <math>D_i</math> is the dark level of the ''i''th pixel. <math>R_i</math> combines the effects of nonuniform illumination and pixel-to-pixel variation in the camera's response. | ||
| + | |||
| + | The goal of flat-field correction is to find <math>I_i</math> for each pixel. The formula for the correction is: <math>I_i = \frac{P_i - D_i}{R_i}</math>. In order to do the correction, you need to find <math>D_i</math> and <R_i>. | ||
| + | |||
| + | <math>D_i</math> can be found empirically by recording a ''dark image'' with the illuminator turned off. Because dark level depends on the exposure, gain, and binning settings, temperature of the detector, and so on…, it is important to take the dark image with identical settings as the source image. It's a good practice to record the dark image just before or after the source image. | ||
{{Template:20.309 bottom}} | {{Template:20.309 bottom}} | ||
Revision as of 02:32, 8 September 2015
Overview
Before you record any images, it is a very good idea to adjust your microscope optics to make the illumination is as good as possible. Even if you adjust the illuminator perfectly, the light intensity won't be exactly the same everywhere in the field of view. In most cases, the illumination is brightest in the middle of the image, with a steady decrease in intensity as you approach the edges of the field of view. Dirt or other flaws in the illumination system can also cause variation in the illumination. Another source of non-uniformity is pixel-to-pixel variation in the dark level and responsivity of the camera. Because of this, even in complete darkness, all of the pixels on the detector will not necessarily report the same value. Identical light intensities may produce different outputs depending on which pixel on the detector records the signal. These problems can be largely eliminated through a technique called flat-field correction or shading correction.
Correcting an image
The value of each pixel in the image is equal to $ P_i = R_i I_i + D_i $, where $ P_i $ is the pixel value recorded by the camera for the ith pixel; $ R_i $ is the responsivity of the ith pixel; $ I_i $ is the intensity of light incident on the ith pixel; and $ D_i $ is the dark level of the ith pixel. $ R_i $ combines the effects of nonuniform illumination and pixel-to-pixel variation in the camera's response.
The goal of flat-field correction is to find $ I_i $ for each pixel. The formula for the correction is: $ I_i = \frac{P_i - D_i}{R_i} $. In order to do the correction, you need to find $ D_i $ and <R_i>.
$ D_i $ can be found empirically by recording a dark image with the illuminator turned off. Because dark level depends on the exposure, gain, and binning settings, temperature of the detector, and so on…, it is important to take the dark image with identical settings as the source image. It's a good practice to record the dark image just before or after the source image.
