1. Open the original observations
Choose an observing sequence from the public archive, or select a ZIP containing your original observations. The workspace inspects the FITS files and identifies the observing settings and available calibration frames. Keep the original file so you can reconnect it if you need it again.
Local execution runs the reduction on your computer. Keep its browser tab open and your computer awake during the calculation. Large sequences use browser storage as well as memory, so available disk space still matters. Server execution runs the reduction remotely. Online services are also used for AAVSO submission and may assist with plate solving.
2. Review the frames and calibration
Look through the sequence for frames affected by clouds, poor tracking, trails, or a target that leaves the image. Review automatic warnings in context and record the reason for any exclusions. Keep enough useful data to describe the observing baseline and the transit.
Use the calibrated preview when compatible calibration is available. A sequence without compatible bias, dark, or flat frames can still have a usable raw preview; that does not mean calibration was applied. LCO BANZAI images already include their archive calibration, which the reduction preserves rather than repeating those corrections.
3. Confirm the target and comparison stars
Check that the selected reference frame, planet name, filter, and observing location match the original data. Plate solving relates image pixels to sky coordinates, helping the workspace locate the target. Verify the marked star against the reference image rather than relying on a plausible-looking light curve later.
Choose comparison stars that are distinct, unsaturated, and usable throughout the sequence. Suggested stars are starting points for that review. A bright star that is saturated or blended with a neighbor may be a poor comparison, and a star near the edge may move out of the field as the telescope tracks.
4. Run EXOTIC and inspect the result
Start the reduction after reviewing the settings and star positions. EXOTIC measures the stars and fits the transit model. The workspace reports progress through preparation, registration, photometry, and fitting; these stages can take different amounts of time.
Compare the model with the measurements and uncertainties. Look at the residuals for structure and at the corner plot for parameter uncertainty. A fitted transit-shaped line is not sufficient evidence that every input choice was correct. Review unexpected scatter, implausible parameters, or missing baseline before submitting.
Download the result package and keep it with your review notes. Results calculated locally must be saved to your account before the online submission service can use them. Continue with the AAVSO guide when you are ready to share the report.
Source documentation
These guides describe the Exoplanet World workflow. Consult the original project documentation for the underlying software and observing program.