Lucky imaging is a highβspeed imaging technique that captures thousands of shortβexposure frames of a turbulent target. By selecting only the sharpest frames, astronomers can approach the diffraction limit of their telescope despite atmospheric seeing.
The selection process inevitably discards a large fraction of the data. Knowing the rejection rate is essential for planning exposure time, data storage, and postβprocessing resources, because the retained frames must still provide sufficient signalβtoβnoise.
The rejection rate (R) is calculated from the total number of frames captured (Ntotal) and the number of frames kept after quality assessment (Nkept). A higher R indicates stricter selection, which improves image quality but reduces total integration time.
What is Lucky Imaging?
How does Lucky Imaging improve astronomical observations?
Why is knowing the rejection rate important in Lucky Imaging?
What factors affect the rejection rate in Lucky Imaging?
Can you explain how the calculator determines the rejection rate?
What are some common applications of Lucky Imaging?
How does Lucky Imaging differ from traditional long-exposure photography?
Results are for informational purposes only and do not constitute professional advice.
