By Greg Parker
This e-book relies round the author's appealing and occasionally awe-inspiring colour photos and mosaics of deep-sky items. The e-book describes how related "Hubble classification" pictures could be created by means of beginner astronomers of their again backyard.
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Additional info for Making beautiful deep-sky images : astrophotography with affordable equipment and software
This being the case, you will find in your imaging that you can use much shorter subs for imaging star fields and clusters than you can in imaging nebulae and galaxies. As a final comment I need to discuss the most contentious issue of all, and that is the question of f# and the “speed” of an optical system. You will see in various places on the web that the “speed”, basically meaning the f# of an optical Assembling your Imaging System 35 system, does not apply to systems using a CCD. This is, in my opinion, complete nonsense I’m afraid.
Again, for autoguiding your refractor, you will have the same three options. A second guide scope (usually a smaller aperture refractor), an off-axis guider with its own guide CCD, or a combined imaging/guiding CCD mounted on your main imaging refractor. Recall that this last combination can cause you trouble when H-alpha, or narrowband filter imaging as you may need long integration times for the guider part of the CCD to detect stars, and this may give an incompatibility with good autoguiding.
Why should this be? You have cantilevered your scope over at some angle dependent upon your latitude, and it wasn’t primarily designed to be as stable in this configuration. Far better that you buy an equatorially mounted scope in the first place if your ultimate intention is imaging and be done with all these annoying little problems! C. telescope itself. Focusing is usually afforded by moving the main primary mirror, and the secondary mirror must be accurately aligned (collimated) to the primary to get the best results from your scope.