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

Local fits do not resolve a Kepler to TESS secondary eclipse change for Kepler-1658

We tested whether the secondary eclipse of Kepler-1658 is larger in seven TESS sectors than in 15 Kepler quarters. We fixed the secondary phase from prior timing. The first test integrates local flux loss over four hours after the archive correction and a quadratic baseline fit. It accepts 103 Kepler and 46 TESS eclipses. The areas are 137.9 and 287.0 parts per million hours. The TESS minus Kepler difference is 149.1, with a conditional 95% t interval from -566.5 to 864.7. An additional fixed-shape fit accepts 212 Kepler and 46 TESS events. It gives depths of 62.0 plus or minus 10.0 ppm and 133.4 plus or minus 78.1 ppm, where the errors come from deleting whole segments. The TESS depth has a conditional 95% interval from -57.8 to 324.5 ppm. All tested shape and baseline variants leave the mission difference unresolved. Joining adjacent TESS sectors into four visits gives the same result with wider intervals. These results assume the stated local models and independent observing segments. The observing years differ, so wavelength and time effects remain mixed. This work does not discover a planet or a stellar binary. It provides new secondary measurements, their precision and limits, and a reproducible comparison. The package preserves all 22 original FITS files, archive queries and hashes, source code, two saved plans, event and rejection tables, controls, signal recovery tests, figures, and reproduction instructions.

Kepler-1658 · KIC 3861595 · TIC 377873569 · secondary eclipse · TESS · Kepler · eclipsing binary · local baseline · crowding correction · reproducible astronomy

Admitted 1 citing publication

References

7
  1. usesCorrected local eclipse areas of Kepler-1658 agree within measured errors in Kepler and TESS data sci:sha256:ff56b87e821622ba402fbc5e6f065a54dc8c6cf0f987c5f78b159a1c76af5498

    We reuse its verified archive FITS snapshot, provenance records, download code, and local area method. We extend the work from primary eclipses to secondary eclipses and add a fixed-shape comparison.

  2. usesdoi:10.3847/1538-3881/ab0e8e

    We use the earlier secondary timing to fix phase and Figure 8 to specify an approximate shape for an additional fit. We compare the recovered Kepler depth with its prior measurement.

  3. usesdoi:10.3847/PSJ/ae21db

    We use the period and epoch in Figure 4. Its stellar binary model explains why the secondary light is a useful test. The binary identification is prior work.

  4. usesdoi:10.17909/T9488N

    We use 15 original Kepler long cadence light curves for KIC 3861595. Exact archive identifiers and hashes are preserved.

  5. usesdoi:10.17909/t9-nmc8-f686

    We use seven original TESS SPOC two minute light curves for TIC 377873569 in sectors 41, 54, 55, 74, 75, 81, and 82.

  6. doi:10.48550/arXiv.2403.01295

    This earlier study includes Kepler-1658 in a Kepler secondary eclipse variability sample. We do not claim the first study of secondary variation.

  7. doi:10.3847/2041-8213/aca47e

    This earlier work used the first three TESS sectors for primary timing and discussed the difficulty of measuring the secondary eclipse.

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