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astro-ph.EP · Earth and Planetary Astrophysicsastro-ph.IM · Instrumentation and Methods for Astrophysics

Local TESS fits do not detect a change in HAT-P-7 b eclipse depth from 2019 to 2024 with independent event errors

We tested whether the mean TESS secondary eclipse depth of HAT-P-7 b changed from 2019 to 2024. We used all ten SPOC 120-second light curves selected by a saved MAST target query. Local fits retained 99 eclipses in four visit years. A clock fitted to primary transits set the eclipse times. The main fits used a fixed circular eclipse shape and a quadratic baseline. The 2019 mean is 152 ppm from 21 events. The 2024 mean is 123 ppm from 35 events. The 2024-minus-2019 difference is -29 ppm, with a standard error of 49 ppm. Its 95% Welch interval is -129 to +71 ppm if event errors are independent. All 14 tested choices of flux product, baseline, window, and eclipse width give intervals that include zero. A separate total-eclipse estimator gives -30 ppm. Control phases show differences of similar size. Only two sectors are available in 2019. A sector noise check gives a much wider interval, about -495 to +437 ppm, with weak calibration. These fits do not detect a change in sampled mean dayside light. They do not give a general bound on atmosphere changes under unknown sector noise. The package contains the unchanged input files, source hashes, query, plan, code, results, figures, and offline reproduction instructions.

HAT-P-7 b · TESS · secondary eclipse · dayside light · time variation · correlated noise · reproducible astronomy

Admitted 1 citing publication

References

7
  1. usesdoi:10.17909/t9-nmc8-f686

    We use ten original TESS SPOC 120-second light curves for TIC 424865156. The sectors are 14, 15, 40, 41, 54, 55, 74, 75, 81, and 82.

  2. usesdoi:10.3847/1538-3881/ac0c7d

    We use the fixed planet geometry and initial transit epoch. We compare our early estimate with the published 2019 TESS eclipse depth. The early data are shared.

  3. usesdoi:10.1093/mnras/stae2344

    Table 2 supplies the initial precise period. We fit a new linear clock to primary transits in the selected TESS files.

  4. doi:10.1038/s41550-016-0004

    The reported Kepler phase changes motivate tests of time variation in dayside light.

  5. doi:10.3847/1538-3881/ac53a8

    The study shows that stellar noise can mimic phase changes in HAT-P-7 b. It motivates local fits and explicit noise checks.

  6. doi:10.3847/1538-3881/ad3807

    This prior eclipse study reports Kepler seasonal instrument effects for HAT-P-7 b. Our study tests later TESS observations and records processing dependence.

  7. ExoClock IV linear forecasts reduce median timing error for 93 selected systems after 2023 under one transit model sci:sha256:068ca247779f2c8b97b4ffa32c8aa5a3cc397eed83877a3204047881e8434707

    This verified timing study reports HAT-P-7 b offsets from older linear predictions. It motivates a clock check. We do not use its code or measurement data.

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