ADVANTAGES OF OUR PARABOLIC TELESCOPE MIRRORS
Our telescope mirrors are manufactured using a proprietary computer-controlled process. A key feature of this method is that during parabolization at low speed and low concentration of polishing material, the polishing tool continuously passes over the entire surface of the mirror, covering all radial areas at each stage of the process.
This ensures a smooth, continuously evolving optical figure throughout parabolization, avoiding the formation of discrete zones or abrupt surface transitions. The resulting parabolic surface exhibits exceptional smoothness, balanced edges, and the absence of zonal errors. Interferometric analysis confirms excellent wavefront slope continuity, with local slope errors maintained below 1 arcsecond and transverse aberrations remaining within the diffraction disk for the specified focal ratio. This level of surface smoothness minimizes scattered light and helps preserve maximum image contrast.
The achieved Strehl ratio is always above 0.95 and typically lies in the 0.97–0.99 range, as documented in our interferometric test reports.
It is important to note that these Strehl values are derived from full-aperture interferometric measurements, which include all surface aberrations across the entire optical area. Unlike tests that evaluate only selected profiles or specific aberrations, interferometry provides a complete wavefront analysis, revealing effects such as zonal structure, edge behavior, and astigmatism that may otherwise remain undetected.
All our mirrors are manufactured from Borofloat® 33 and Supremax® glass produced by SCHOTT (Germany) and are delivered with a full interferometric test certificate. With a thickness of 25 or 38 mm, the mirrors are lightweight and reach thermal equilibrium rapidly, contributing to stable optical performance during observation.
PRIMARY MIRROR 205 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 255 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 300 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 355 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 400 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 460 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 510 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 560 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
PRIMARY MIRROR 600 mm
- Strehl ratio ≥ 0.95 (typically higher)
- Full-aperture interferometric test with certificate included
- Contact us for prices of any diameters which is not listed here or for thicker mirrors.
- Here you can see the independent test results of two of our telescope mirrors. The test is made by the famous expert Wolfgang Rohr.
Edge Finish
Mirrors with a 25 mm thickness are supplied with rough edges left from the waterjet cutting process. This is a normal manufacturing characteristic and has no impact on the optical quality or performance of the mirror.
Mirrors with a 38 mm thickness and above are supplied with precision-ground, smooth edges as part of the finishing process.
REFIGURING OF FINISHED TELESCOPE MIRRORS
We offer interferometric testing and refiguring of finished telescope mirrors. The scope of refiguring and the final cost depend on the optical condition of the mirror and the corrective steps required. Depending on the initial surface quality, the process may involve complete regrinding, polishing and parabolization, or only polishing and parabolization, or in some cases parabolization alone. The required corrective stages are determined after a preliminary interferometric test, which is always performed before any refiguring work begins.
The images show the surface condition of a mirror before and after refiguring, illustrating the improvement achieved through the process.
BEFORE REFIGURING
Strehl = 0.766
