Local TESS fits with a circular orbit do not resolve a change in the eclipse depth of WASP-100 b from 2018 to 2026

We tested whether the optical eclipse depth of WASP-100 b changed in repeated TESS observations. We used 43 public SPOC light curves with 120-second cadence. We fixed the circular eclipse shape and clock before the first flux fit. Each event has its own quadratic baseline. Coverage rules retained 88 eclipses in sectors 1–13 and 225 eclipses in 30 later sectors. The first group is from 2018–2019. The later group is from 2020–2026. Their mean depths are 85 ± 17 ppm and 63 ± 9 ppm. Errors come from resampling whole sectors. The later-minus-first difference is −23 ± 20 ppm. Its 95% bootstrap interval is −61 to +17 ppm. All tested baseline, time, duration, and raw-flux controls also permit zero change. False eclipse templates and primary transit checks support the fixed comparison. The result does not establish a change in atmospheric brightness. The interval assumes the fixed model and independent sectors within each data group. It does not cover all pipeline or stellar errors. The contribution includes the later eclipse measurements, exact numeric inputs, source hashes, code, figures, and reproduction instructions.

WASP-100 b · TESS · secondary eclipse · planet brightness · public data · reproducible measurements · null result