![]() where one cannot neglect the dark noise over the sky noise, the ideal single exposure time is half as long as with a cooled camera. In the low-light regime, the significant noise sources are read noise and dark current noise. Noise sources in CCD cameras add in quadrature (the square root of the sum of the squares). Since dark current noise follows Poisson statistics, the rms dark current noise is the square root of the dark current or, in this case, 2 e-/p. So, I interpret this that with an uncooled camera under very dark skies, i.e. For a 4-second exposure, a total of 4 electrons/pixel are generated (1.0 e-/p/s x 4 sec). We have assumed that we have measured the read noise of the sensor to be \sigma_r, so we can use the rule of adding in quadrature to get the total noise for the frame Typical bias current of FET input amps is about 1 pA, which equals 0.57 fA/Hz. ![]() For a large pixel (24 x 24m2), we can reach a. (SF), it aims to buffer the voltage and amplify the current. The dark current is expressed in current density A/m2 or in electron/pixel/second e -/pix/s (Fig.15). ![]() I took the liberty to use the extensive description of yours in viewtopic.php?f=35
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