WHAT YOU NEED A FOUCAULT TESTER: For those who still do not know; It serves to apply the Foucault test on an optical surface, parabolica, reflective, under construction, to infer the fixes to be implemented in order to bring it in to a most high quality. Given that in a parabolic mirror, the radius of curvature of the surface increases
To obtain good interference fringes, for the control of optical surfaces, through the so-called "test plate", It is necessary to have a 'apparatus allowing to uniformly illuminate, with a monochromatic light, the two glasses under test and redirect the resulting image at the device or towards the observer. The device itself is
In this article I will explore with a question of interpretation of the interference fringes, by means of the interferometer Newton, during the analysis of the optical surfaces. As I described in this article, the evaluation of the profile of the convex surface is performed picking her compare with a reference surface (concave) that can be spherical, parabolic or
In this short article, I would like to start introducing the Hartmann test, beginning to describe the principles of operation, the merits and defects, paving the way for further developments and modifications to be able to easily use on the part of us amateur accomplishments during grattavetro. The Hartmann test was invented by Hartmann (1900) per
Is’ born in 1939 and it serves to measure with extreme precision (impossible to Foucault test for reasons which we shall see here later looking at the title: REASONS WHY THE FOUCAULT TEST IS INACCURATE FOR LOW FOCALS RATIOS MIRRORS)) the radii of curvature of the zones of a parabolic mirror, or even more deformed figure from, a very short focal ratio (that is more inferior to F5) and a beyond the diameter 300 or
The subject self-build a telescope, at a certain point of its progression it leads to make concatenated choices, where the pupil of the eye conditions the determination of the minimum magnification with an eyepiece "telescope finder" or wide field; from which it is derived the design of the full light field" (Field Of View) be prepared, and then the
With the previous article we saw the mirror 200F6 working with parabolization's corrections derived from five successive retouch actions and following Foucault tests controls. With this article we will see the remaining 5 tweaks that will bring us to the end of the mirror processing. Obviously, this continues to be a realistic simulation of the cases in which
Now that, with previous articles we did a little 'light on the road to complete the construction of a mirror, we walk that way "that becomes increasingly narrow and challenging" parabolizing slowly with a slow progression of quality. Obviously this is a simulation of what would happen in reality, but it is
In order to facilitate an excellent evening observing through a telescope, We know that this must be in perfect conditions of stability, and collimation and thermal equilibrium. This last issue will be analyzed in this post, to highlight what are the main parameters affecting the optics acclimatization time, the possible measures to improve the problem and
Hartmann test (simplified by Mirco)
As mentioned in the preceding article (Hartmann test) in this post I describe the method which I have recently begun to be used to test the optical during processing and which is based on the Hartmann test. In the mirror parabolizzazione phase, in particular the last stage of refinement of the shape of the surface it is necessary to know with precision
Read More