Friction Mount Twinstar FG80

Achieving sub-arcsecond level tracking precision is not just a promise but a reality with our friction drive system. Free from the complexities of encoders and elaborate electronic setups, our technology provides a direct and efficient solution for astronomers who prioritize precision without compromising simplicity. Say goodbye to the challenges associated with intricate electronics and software—our friction drive system empowers you to focus on the beauty of the cosmos rather than navigating technical complexities. The absence of encoders doesn’t hinder performance; instead, it enhances the reliability and ease of use of our system.

Overall, the mount-based of the friction-based drive is extremely precise in pointing, too. It’s crucial to note the significant advancements in recent blind plate solving solutions. These software-based solutions, often freely available, have the capability to achieve sub-arcminute level positioning swiftly, without requiring substantial investments. This allows for enhanced accuracy and efficiency in astronomical observations within minutes.

In the realm of telescope mounts, particularly in higher price ranges, the prevalent trend involves reliance on encoders. This is often necessitated by mechanical imperfections in the drive system, requiring encoders for accurate tracking and position monitoring. However, the use of encoders contributes significantly to the overall cost of these mounts.

Precise encoders themselves come with a hefty price tag, sometimes reaching a few thousand euros for just one. Additionally, specialized electronics and software are essential for constant correction calculations. While mounts equipped with encoders indeed offer sub-arcsecond level tracking precision, this comes at a considerable cost.

The Twinstar team has developed a unique drive system that achieves the highest precision without relying on expensive and vulnerable encoders and electronics. This innovative solution ensures accuracy without compromising on cost or durability.

Our telescope mount consistently delivers exceptional tracking precision, maintaining an accuracy of 0.5 arcseconds for an unlimited duration, with minimal deviation. This level of precision ensures that your observations and astrophotography sessions are highly reliable, even over extended periods.

We recommend using longer exposure times or implementing a variable exposure delay in PHD guiding software. This approach allows the guiding system to average out seeing conditions and reduce the impact of short-term atmospheric disturbances.

Seeing Conditions: It’s important to note that seeing conditions—the atmospheric turbulence that can blur astronomical images—are typically the primary factor affecting tracking precision. Even with our highly accurate tracking capabilities, the quality of your observing location and the current seeing conditions will significantly influence your results.

A typical PHD guide graph made with an FG80 mount loaded with 50 kg (telescope tube + counterweights) under moderate seeing conditions would show relatively consistent guiding with some fluctuation, primarily due seeing conditions.

In most observing scenarios, particularly if you’re not at a location with excellent seeing conditions, you will find that our mount’s tracking precision far exceeds the demands of your observations or astrophotography.
By following these guidelines and taking advantage of the mount’s precision, you can achieve outstanding results, even under challenging conditions.

A practical hint for determining the Minimal Guide Scope Focal Length

The Minimal Guide Scope Focal Length refers to the shortest focal length that a guide scope should have to ensure accurate guiding during astrophotography or tracking. This is important because the guide scope needs to accurately detect small movements of a guide star to keep the main telescope focused on the target.

Where:

• Main Telescope Focal Length is the focal length of your primary imaging telescope (in mm).
• Guider CCD Pixel Size is the pixel size of the camera used in your guide scope (in microns).
• Main CCD Pixel Size is the pixel size of the camera used in your main telescope (in microns).

This calculation ensures that your guide scope can detect small enough deviations in star position for accurate guiding.