Your UV Mirror Questions, Answered (Astronomical Telescopes)

Every Astronomical Telescopes system eventually meets the same question: where does the light go, and how much of it survives the turn? A well-specified UV Mirror…

Every Astronomical Telescopes system eventually meets the same question: where does the light go, and how much of it survives the turn? A well-specified UV Mirror answers both, which is why it earns a place on the bill of materials long before the enclosure is drawn.

Think of the UV Mirror as a precisely made fused silica or calcium fluoride plate whose working surface is a UV-enhanced dielectric or aluminum. The result is > 90% in the UV reflection across 193–400 nm, which is exactly what most Astronomical Telescopes builders are looking for.

When light meets the UV Mirror, almost all of it bounces from the front coating. The substrate merely holds the coating in place; it does not need to be traversed by the useful beam, so transmission losses and secondary reflections stay minimal — a real advantage in sensitive Astronomical Telescopes setups.

Most of the engineering in a UV Mirror lives in its UV-enhanced dielectric or aluminum. The stack is designed for 193–400 nm and delivers > 90% in the UV, and its environmental protection layer keeps the metal from tarnishing so the mirror keeps working year after year.

A UV Mirror starts as a fused silica or calcium fluoride blank. We hold it to λ/10 flatness and 20-10 surface quality, then apply the UV-enhanced dielectric or aluminum. The substrate never sees the beam directly, but its figure sets the limit on how straight the reflected wavefront stays.

A practical UV Mirror datasheet reads: fused silica or calcium fluoride substrate, λ/10 flatness, 20-10 quality, 1–5 mm thick, > 90% in the UV over 193–400 nm. Those five lines settle most design reviews for Astronomical Telescopes. See the standard size list for what we stock and what we cut to order.

Where folding long optical paths inside compact tubes, a UV Mirror earns its place by doing one job reliably: turning the beam without adding noise. In Astronomical Telescopes that reliability is the difference between a prototype and a shippable product. More application examples are worth a look if the use case is close to yours.

Quick answers

How thick should it be? 1–5 mm covers most needs; thicker helps rigidity. Is the coating durable? The protective layer on a UV-enhanced dielectric or aluminum is meant for normal lab and instrument use. Can I get a non-standard size? Absolutely — we cut to ±0.01 mm in mm or inches.

Selecting a UV Mirror for Astronomical Telescopes starts with the wavelength and angle of incidence, then the acceptable loss. Match the UV-enhanced dielectric or aluminum to 193–400 nm, confirm > 90% in the UV, and make sure the fused silica or calcium fluoride and 1–5 mm fit the mount you already have. The spec and size tables make that comparison quick.

Mirrors reward careful handling. Hold a UV Mirror by the edges, keep the coated face away from fingers and aerosols, and clean only with approved optics tissue and solvent when truly needed. Store it in its packaging, coated face protected, and it will hold > 90% in the UV for years.

At JYOPTO we make UV Mirror parts by cutting fused silica or calcium fluoride with laser accuracy of ±0.01 mm, then applying the UV-enhanced dielectric or aluminum under vacuum. Standard blanks run 1–5 mm thick, edges are smoothed for safe handling, and every shipped mirror meets λ/10 flatness with a 20-10 surface — the same disciplines we apply across our optical glass, vacuum-coating and precision cold-processing lines since 2020.

Environment matters. A UV Mirror headed for Astronomical Telescopes may see condensation, vibration and frequent handling. Specifying a sealed-edge, protected coating and a stable fused silica or calcium fluoride substrate means the mirror keeps its figure (λ/10) and its reflectance through warranty periods and beyond.

For Astronomical Telescopes, do not over-specify. Choose the UV-enhanced dielectric or aluminum that covers 193–400 nm at the angle you use, keep flatness at λ/10 unless the wavefront demands more, and you will have a UV Mirror that is both capable and economical.

At JYOPTO we make UV Mirror parts by cutting fused silica or calcium fluoride with laser accuracy of ±0.01 mm, then applying the UV-enhanced dielectric or aluminum under vacuum. Standard blanks run 1–5 mm thick, edges are smoothed for safe handling, and every shipped mirror meets λ/10 flatness with a 20-10 surface — the same disciplines we apply across our optical glass, vacuum-coating and precision cold-processing lines since 2020.

A UV Mirror starts as a fused silica or calcium fluoride blank. We hold it to λ/10 flatness and 20-10 surface quality, then apply the UV-enhanced dielectric or aluminum. The substrate never sees the beam directly, but its figure sets the limit on how straight the reflected wavefront stays.

A UV Mirror is an optical component built so that reflection happens at the coated front face rather than through a substrate. With a UV-enhanced dielectric or aluminum on a fused silica or calcium fluoride base, the part delivers > 90% in the UV reflectivity across 193–400 nm while keeping the useful aperture clean and ghost-free.

The UV-enhanced dielectric or aluminum is where performance is won or lost. Deposited by vacuum processes, it is tuned so the reflected wave adds constructively across 193–400 nm, reaching > 90% in the UV. Getting the layer thickness right is a precision task: a few nanometers off and the reflectivity curve shifts.

For Astronomical Telescopes, do not over-specify. Choose the UV-enhanced dielectric or aluminum that covers 193–400 nm at the angle you use, keep flatness at λ/10 unless the wavefront demands more, and you will have a UV Mirror that is both capable and economical.

The UV Mirror is not exclusive to Astronomical Telescopes. Universities, service centers and R&D groups use it wherever a beam must turn, which makes a flexible, customizable part a quiet workhorse across the optics world.

The UV Mirror is not exclusive to Astronomical Telescopes. Universities, service centers and R&D groups use it wherever a beam must turn, which makes a flexible, customizable part a quiet workhorse across the optics world.

Quality control

Every UV Mirror is measured, not just sampled. Flatness against a reference, scratch-dig against 20-10, and a reflectance spot-check at 193–400 nm confirm the UV-enhanced dielectric or aluminum performed as designed. Documented results matter most for Astronomical Telescopes, where one bad part can stall a whole instrument.

Typical specs worth putting on a drawing: surface flatness λ/10, surface quality 20-10 (scratch-dig), substrate fused silica or calcium fluoride, thickness 1–5 mm, and reflectivity > 90% in the UV over 193–400 nm. Stating these up front saves rounds of sampling later. Our full technical specifications and standard sizes list the tolerances we hold routinely.

In short

For Astronomical Telescopes, the UV Mirror is less a commodity than a tuned component. Specify the band (193–400 nm), the reflectivity (> 90% in the UV) and the figure (λ/10), and you will spend less time debugging light you cannot see. That is the whole game. Where your application sits among the sectors we serve changes the details, not the method.