A new method for observing large areas with physically small detectors, which are unable to cover the whole area simultaneously, based on multiplexing several scanned areas onto a single detector unit followed by algorithmic reconstruction of the true field of view.
Astronomical observations require the ability to detect very weak signals at high spatial resolution. This reflects on the special characteristics of the observation systems; they need to have a large aperture, high resolution detectors and very low system noise. These demands render high costs and complexity.
Our multiplexing and reconstructing method was developed based on the sparse nature of astronomical observations, and it could be implemented in any application in which sporadic data points are to be found against a fixed (whether detailed or blank) background.
- Highly efficient telescopes
- Quick quality assurance systems fault metrology
- Implementation in microscopy
- Use of small size detectors
- Ability to scan large fields (compared to detector size)
- Maintaining high resolution
- Significant shortening of scan time
- Easily applicable to existing systems
The method was developed for astronomical observations in which the studied field is immense and the detector size is relatively small and limited. The invention consists of an optical system that directs light (IR, Vis, UV or other) from different locations in the sky to the focal plane of a telescope onto a specific single detector area, creating a multiplexed image in which several portions of the sky are presented collectively.
Such multiplexing is done on each detector unit area with a different set of sky loci.
A reconstruction algorithm was developed to construct sub-observations sets in a method that guarantees unique recovery of the original wide-field image even when objects overlap.