To try and sum it up, the aperture of a scope determines its resolution. This is often expressed as the scope's "Dawes Limit" (R=11.6/D - the smallest distance two identical point sources, like the components of a double star, can be separated: R in arc seconds where D is the scope's aperture - diameter - in cm)
If the image scale of the sensor's pixels matches the Dawes limit of the scope (e.g. each pixel covers the same number of arc seconds in the sky as the scope's Dawes limit) w'd say that the aperture is perfectly sampled: some sensors on some scopes can be oversampled (the pixels in the sensor are smaller than the scope can resolve even in perfect conditions) or undersampled (the pixels are bigger than the scope's Dawes limit so limit the resolution of the scope). the total number of pixels will determine the size of the field (more pixels - or megapixels - on the same scope will cover a bigger field)
That's all in perfect conditions, which never happen. The scope might be less than perfectly in focus across the whole field, or there might be other aberrations which have the effect of blurring things, or the atmosphere has many ways of doing that too. That often means that some undersampling is fine in practice: the scope is rarely or ever going to be able to resolve to its Dawes limit so although the sensor is theoretically limiting resolution, in practice it is not. Larger pixels are easier and cheaper to make, and tend to be less noisy, so many manufacturers will tend to allow some undersampling when they match a sensor to a scope.
All real scopes, and smart scopes, are compromises between many competing factors. The best are those that balance these to give good results on the intended targets. Current smart scopes simply are not designed to be useful for planetary imaging but tend to be fairly fast, and fairly wide-field, to work well on the larger DSOs.
Edited by chrisecurtis, 10 January 2025 - 04:49 PM.