6/16/2023 0 Comments Focal length on astrometry![]() The inherent defects in the sensors are different: we no longer have hot CCD pixels, but we see “telegraph noise” appear, which can give an outlier to a given pixel in a given image. This effect is more or less corrected according to the manufacturers.Ħ. This results in bright areas in the image. We also see on CMOS sensors a phenomenon called “Amp glow”, linked to thermal sensitivity. The thermal signal, which had almost disappeared with the latest CCDs, reappears on CMOS, which requires effective cooling to keep the same level of performance.ĥ. ![]() ![]() The reading dynamic is lower (for the moment) in CMOS (12 bits in CMOS instead of 16 bits in CCD in most cases).Ĥ. CMOS camera pixels are generally smaller.ģ. In fact, there are still notable differences:ġ.The price of CMOS sensors is significantly cheaper than CCDs.Ģ. The cameras that are within our reach are now all in CMOS technology this change in technology gives us the opportunity to look in detail at the selection criteria for such a camera.Īt first glance, CMOS technology completely replaces the CCD, with no apparent effect on the user. The range of guiding cameras is constantly evolving, and the CCD cameras that we recommended a few months ago (Atik Titan and 314L +) are no longer available today. We must never forget that what differentiates a “beautiful” observation from a bad observation is only the amount of light injected into the spectroscope! In astronomical spectroscopy, guiding camera is an important element, since it’s what makes it possible to point the right target (star, nebula, etc.), then to ensure precise guiding to inject the maximum light into the spectrograph slit.
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