Seestar Photometry Analyzer
Explore stellar brightness measurements directly in your browser.
Drop Seestar photometry CSV files here, or select files from your device.
Try a fictional star: six hours of simulated observations, with a 0.65 mag eclipse-shaped dip and recovery.
Download the CSV, then select it above. Educational simulation · not real observations.
Your observation files remain on your device. All calculations are performed locally in your browser.
Session evidence · experimental field analysis
First load a dedicated target log above and select its target below, then scan its session folder to check the supporting measurements. You can also scan without a log for a file and measurement inventory.
Reads one CSV at a time. Originals are never changed or copied. FITS and JPEG files are counted only; image data is not loaded. Copy a completed observing session locally with Finder or Explorer first.
No folder scanned.
Field stars · provisional associations
Scan a session folder to build coordinate-based tracks.
Positions within 3 arcseconds of a running centre can join a track only when the match is unambiguous in that exposure. Nearby competing detections are left unassigned. IDs stay fixed within this scan; new scans rebuild them. Coordinate labels are not catalogue identifications. A track can still split or contain a mistaken match. No eclipse or physical variability is confirmed.
Light-curve gallery
Uses the star search and minimum-observation filters above. Each thumbnail shows unfiltered 5-minute medians, centred on the star's median, over the same session timeline. Fainter is lower. Gaps over 15 minutes are disconnected. Click a curve to inspect it.
Review priority is robust binned range relative to scatter, reduced for sparse coverage. It is not an eclipse probability or a matching-quality score. Track fragments and instrumental effects can rank highly. Auto-scale can exaggerate small changes.
Catalogue lookup · on request
First plot a field star, or load and select a target log. Local lookup reads only nearby ASTAP .1476 cells, within 10 arcseconds. No ASTAP application is needed. These compact catalogues provide positions and magnitudes, without star names. SIMBAD opens an external service only when you click its link, sharing the position and search radius.
No local database selected.
Checking saved folder selections…
Stores folder access handles in this browser, not observation contents. Nothing is read automatically on reopening the app. Use a Reopen button to start; the browser may request read permission again. Remembered folders may be unavailable in private browsing, after clearing browser data, or if the drive is disconnected.
Stellar light curve
Actual observation times · inverted magnitudes · clock-aligned medians
Variability screening awaits observations.
How variability screening works
This conservative heuristic looks for same-direction median changes across at least three consecutive bins, each containing at least three retained measurements. The total change must exceed the larger of 0.05 mag, three times the median reported uncertainty, or three times the median within-bin sample scatter. Gaps break a trend. It can miss real events, especially reversals, noisy curves, or sparse data, and can flag instrumental trends. It does not estimate statistical significance, confirm an eclipse, or forecast a recurrence. Results depend on bin size and quality filters.
Tracking Diagnostics
Reported sensor coordinates can reveal drift and sudden movement. A flagged change is a possible movement event; it does not prove a telescope slew or invalidate a measurement.
Statistics and exports use retained measurements. The observation panel summarizes all valid, timed magnitudes for the selected target. No interpolation is applied.
| Bin start (recorded clock) | N | Median mag | Mean mag | Sample SD | Mean SNR |
|---|