Click on the picture to see a movie of a grinding machine in action.
Click on the picture to see a movie of a grinding machine in action.
Your primary mirror is eight(8) inches wide; and it has a 80 inch focal length.
So, your telescope is an f/10. Your maximum useable eyepiece focal length would be 60mm (from 10x6=60). And the highest power eyepiece you should use would be a 6mm focal length (from 60/10=6). This telescope will use a wide range of eyepieces, but nothing less than 6mm is worth trying if the conditions are short of spectacular.
This can help you save $$ [by not buying eyepieces which won't work on your telescope] and time.
When the two formulas are combined (since Mag1=Mag2); we get:
(Entrance)/(Exit)=(Telescope FL)/(E.P. FL)
or, (E.P. FL)=(Exit)*{(Telescope FL)/(Entrance)}
Which boils down to...(E.P. FL)=(Exit)*(F-ratio)
Entrance Pupil = your telescope's largest diameter
Exit Pupil = your eye's widest diameter {usually 6mm}
The nice part is this works for any telescope!
Some 6-inch Flats that I made:
Click on each picture to see how the final mirror came out (Note: The final pictures all used a monochromatic mercury light source.)
The background light is monochromatic (sodium line). Using an interferometer, you may "see" the flatness between two mirrors. Between each interference line there is 1/2-wavelength of seperation between the two surfaces. This causes a "topographic relief map" of the combination to appear.
You can think of flats as mirrors with infinite focal length. However most flats do not have focal lengths quite that long. The focal length will depend on whether the average surface departure is convex or concave, and the diameter of the mirror. It is easier (and more correct) to grade a flat by the amount that it's surface departs from being flat in degrees of wavelength (for the given color used to test the flat).
The surface of mirror "C" was within 1/16 wave of being flat; "A" was 1/8 wave; and "B" was nearly 1/4 wave. This describes the average surface "flatness". With the proper test equipment, mirrors of extremely small surface errors (1/20-wavelength or less) may be measured.
By equating their relative interference patterns to equations {A + B = %-of-half-wave, etc.}; it is possible to build a matrix to solve for the three surfaces in terms of their percentage of a half wavelength.
This was a really fun project, but it took me forever to finish the flats. It was a lesson in patience and thought.
Click on pictures for additional info.
An MTF (Modulation Transfer Function) is a fancy way to show you how your optics will perform (or not) if you were to look at a test pattern of alternating white and black stripes. This is confusingly called "CYCLES/MM" in the graph. I have set the scale so that each increment represents 1000 alternations per inch (or 39.37 Cyc./MM). As you can see, the telescope image on axis will pass 50% of it's image past the 2000 Alt/in. While the off axis image (in this case the outter edge of Saturn - dia.=20arcsec) will easily pass 50% of that image at a resolution of 500 Alt/in. The typical human retina will be able to resolve the entire image (it usually starts in the lower left hand corner and arcs upward to cross the "perfect" line at 50% - which occurs near 3000 Alt/in.) If you simplify this and draw a straight line from the lower left corner to the midpoint of the "perfect" line you will find that the outter image edge will pass above the 1000 Alt/in. mark; and should be resolved by the typical retina. For a very nice explanation of this go to: http://www.normankoren.com/Tutorials/MTF.html
The TFMTF (Thru Focus MTF) graph is another way to confirm what the SPOT graph shows. The transfer is 90%+ for "on axis" image as well as the "outter edge" image at " zero focus". As in the SPOT graph, I have made the IN and OUT focus range +/- 1/4-inch.