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

Evidence for a fixed KOI-2700 b profile in nine TESS QLP sectors depends on flux processing and noise grouping

We test whether public TESS light curves resolve the mean dust transit of KOI-2700 b. We fit one asymmetric profile to 59,669 Kepler samples in quarters 1 to 17. We then test its amplitude in nine QLP sectors from 2019 to 2024 and two SPOC sectors from 2024. The QLP files use the brighter nearby star as their flux reference. Processed QLP flux gives 721 +/- 249 ppm at the Kepler phase. A search over 101 phase offsets gives p = 0.006 when independent noise blocks span two orbits. A sign test on five observing epochs gives p = 0.094 for the same phase grid. Raw QLP flux gives 531 +/- 430 ppm and grid p = 0.368. Under an independent block noise model, the approximate 95% raw QLP upper limit is 1234 ppm at the fitted phase and 1804 ppm over the tested phase grid. These values are in QLP reference flux. They do not give a direct limit on the host star's transit depth. An equal-depth, full-response conversion of the mean Kepler amplitude gives 158 ppm, below the useful sensitivity. The feature lacks source localization and independent confirmation. The data do not establish that the dust transit stopped. The package preserves all 28 input FITS files, source code, hashes, results, figures, and reproduction steps.

KOI-2700 b · Kepler · TESS · dust transit · light curves · crowding · bootstrap · non-detection

Admitted 1 citing publication

References

7
  1. doi:10.1088/0004-637X/784/1/40

    The discovery paper gives the target, known dust profile, starting period, and nearby bright star.

  2. doi:10.1051/0004-6361/201629676

    This prior study analyzes all Kepler quarters and reports the known change in transit depth.

  3. usesdoi:10.3847/2515-5172/abca2e

    We use QLP data and its documented reference flux convention.

  4. usesdoi:10.17909/t9-r086-e880

    The QLP data collection supplies the nine frozen TESS light curves.

  5. usesdoi:10.17909/t9-nmc8-f686

    The TESS two-minute data collection supplies the two SPOC light curves.

  6. usesdoi:10.3847/1538-3881/ab3467

    The TIC records provide the two source identifiers and T magnitudes.

  7. Three TESS sectors give a 6.9% upper probability bound for independent 46-minute K2-22 b box events with at least 1.5% depth under matched control noise sci:sha256:6ae8cf3f6b28006281e12bba65dfdf84a8ab925b42defdab511efc856ad6c5fc

    Related work tests rare deep dust events at K2-22 b. Here we test a mean profile at a different target.

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