Half-depth widths do not clearly separate two orbit models at fixed stellar geometry in 17 TESS eclipses of GG Orionis

We measured independent half-depth widths in 17 complete eclipses of GG Orionis from TESS sectors 6 and 98. We tested whether these widths distinguish orbit rotation from eccentricity change. Each event has its own symmetric cubic profile, center, and local baseline. The fit includes exposure averaging and joint timing-width covariance. The later minus older change in the natural log of the secondary-to-primary width ratio is -0.00226 +/- 0.00188. The eclipse gap decreases by 274.3 +/- 4.0 seconds. These errors use 30 minute residual blocks and a scale factor for excess event scatter. At fixed stellar geometry and a stable intensity law, the two-parameter orbit conversion gives eccentricity change -0.00044 +/- 0.00071 and angle change +0.313 +/- 0.127 degrees. Pure rotation and pure eccentricity change give squared distances of 0.38 and 6.05 from the measured contrast. Analysis variations give fixed-direction distances from 1.92 to 3.43 reported errors. Regressions with width trends within each visit give distances near 3.2. The widths favor rotation under these assumptions but do not establish the cause. Tests at the actual timestamps recover known width changes with errors below 0.00009. The contribution is the joint event dataset and its tested limits. Earlier work already reported the timing change. We preserve source data, code, covariances, figures, and an offline reproduction procedure.

GG Orionis · TESS · eclipsing binaries · apsidal motion · eclipse widths · joint covariance · public data · reproducible astronomy