Handbook for
Opinions vary as to the utility of flip mirrors. They are a convenient way to find and focus, but they add quite a bit of extra length between the camera and telescope. This can be very inconvenient with Newtonians, and not a lot better with SCTs, especially if the assembly is somewhat flexible. They also make it difficult to use a focal reducer with your camera, as the rapidly converging light cone from a reducer cannot reach all the way through the flip mirror unit to the CCD surface. If you are using one of the popular F3.3 compressors for deep sky imaging, you will NOT be able to include a flip mirror unit in front of your camera and a
Whichever device you use, it is necessary to set up a good optical match between your MX5C and the telescope. Most SCTs have a focal ratio of around F10, which is too high for most deep sky objects and too low for the planets! This problem is quite easy to overcome, if you have access to a telecompressor (for deep sky) and a Barlow lens for planetary work. The new Meade F3.3 compressor is very useful for CCD imaging and I can recommend it from personal experience. It does not require a yellow filter for aberration correction, unlike some other designs, so it can be used for colour imaging. Barlow lenses are less critical and most types can be used with good results. However, if you are buying one for CCD imaging, I recommend a 3x or 5x amplifier, or the planets will still be rather small in your images. As a guide, most CCD astronomers try to maintain an image scale of about 2 arc seconds per pixel for deep sky images. This matches the telescope resolution to the CCD resolution and avoids ‘undersampling’ the image, which can result in squa re stars and other unwanted effects. To calculate the focal length required for this condition to exist, you can use the following simple equation:
F = Pixel size * 205920 / Resolution (in arc seconds)
In the case of the
F = 0.0096 * 205920 / 2 | = 844mm |
11