Four TESS visits of 55 Cancri e do not require a change in mean eclipse depth with a fixed circular orbit

We tested whether the mean optical eclipse depth of 55 Cancri e changes between TESS sectors 21, 44, 46, and 72. We fit 113 events from four public 120 second SPOC light curves. Each event has a local quadratic baseline and a fixed eclipse shape for a circular orbit. Negative depths are allowed. We estimate visit errors by resampling event records in circular blocks. With blocks of four events, the visit depths are 14.80 ± 5.46, 2.84 ± 5.12, 11.23 ± 3.79, and 7.38 ± 5.64 parts per million (ppm). A centered bootstrap test for equal visit means gives Q = 2.987 and p = 0.405. For block lengths 1, 2, 4, and 8, p ranges from 0.216 to 0.583. No tested eclipse fit choice and block length rejects equality at the nominal 0.05 level. The pooled depth depends on the baseline: it is 9.37 ± 2.39 ppm for a ±0.18 day quadratic window and 4.02 ± 2.93 ppm for a ±0.12 day window. The same 113 events enter both fits. A later paired comparison gives a wide-minus-short difference of 4.25 ± 2.02 ppm when the main visit weights are held fixed. This independent analysis agrees with prior four-sector work and adds a reproducible event dataset and method sensitivity tests. It does not establish constant brightness or identify a physical cause. The block errors assume representative within-visit noise and have limited calibration with 23–32 events per visit. The package contains raw FITS inputs, source URLs and hashes, the event inclusion table, all fit variants, code, figures, and run instructions.

55 Cancri e · TESS · secondary eclipses · optical photometry · event resampling · baseline sensitivity · reproducible research