Telescope Mount Model Alignment Without GPS
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Solution Overview
Problem
Conventional telescope alignment methods require knowledge of local time and location, rely on bright stars, and need additional equipment like GPS and digital compasses, making them complex and prone to failure in situations where bright stars are not visible.
Innovation Solution
A method that generates a mathematical transform, or 'mount model,' to align a telescope without knowing the actual local time or location, using arbitrary time and location values, and iteratively refines the Local Sidereal Time (LST) and latitude to minimize pointing errors, eliminating the need for user input and additional hardware.
Engineering Contradictions & Design Principles
Engineering Contradiction Analysis
1Reliability
If conventional alignment methods using bright stars are used, then alignment accuracy can be achieved, but the system fails when bright stars are not visible and requires additional GPS/compass equipment
Solution Approach 1:
The patent extracts the dependency on bright stars and GPS/compass equipment from the alignment system. By using arbitrary time and location values combined with iterative RMS error minimization, the system achieves alignment without these external references, thereby improving reliability in conditions where bright stars are not visible while eliminating the need for additional GPS and digital compass hardware
Solution Approach 2:
The telescope alignment system performs self-service by using its own image capture device to detect stars and automatically calculate alignment parameters through iterative RMS error minimization. The system determines its own time and location information without external GPS or compass inputs, and automatically adjusts mount model parameters based on captured star field images, eliminating the need for user intervention or additional specialized equipment
2Extent of automation
If GPS, digital compass, and accelerometer are added for automatic alignment, then alignment automation is improved, but device complexity and cost increase
Solution Approach 1:
The patent makes the image capture device perform multiple functions: it captures star field images for alignment determination, detects star positions for coordinate transformation, and provides feedback for iterative RMS error minimization. This multi-functionality achieves automatic alignment without adding GPS, digital compass, or accelerometer components, thereby maintaining automation while reducing system complexity and cost
Solution Approach 2:
The system uses its existing image capture device to perform all alignment functions without requiring external specialized equipment. The telescope automatically captures images, processes star positions, calculates mount model parameters through iterative optimization, and adjusts its own positioning, achieving full automation using only components already present in the telescope system
3Measurement precision
If multiple sensing iterations are performed to locate bright reference stars, then alignment accuracy is improved, but alignment time increases
Solution Approach 1:
The patent performs preliminary action by using arbitrary time and location values to generate an initial mount model before actual alignment. This preliminary model serves as a starting point for iterative RMS error minimization, allowing the system to quickly converge to accurate alignment parameters without requiring multiple time-consuming sensing iterations to locate bright stars, thereby reducing alignment time while maintaining precision
Data Source
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AI summary
According to various embodiments, a telescope is automatically aligned without requiring user intervention and without requiring knowledge of actual local time or location. A mount model specifying a relationship between a telescope's internal coordinate system and a celestial coordinate system is generated using an arbitrary time, arbitrary telescope location, and a number of alignment reference points. A pointing error for the initial mount model is determined, for example using a plate solving technique to translate between plate coordinates and celestial coordinates for the alignment reference points. Time and location values are iteratively adjusted to reduce the pointing error until it is acceptably low. In one embodiment, adjustments are made by reference to a local sidereal time (LST) offset and/or a latitude value. In one embodiment, the iterative adjustment is performed using a two-phase methodology, including a coarse adjustment followed by a fine adjustment.