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

Constant period masks need widths above 1.5 durations for 23 of 1,096 selected Kepler planets with fixed event numbers and durations under bounds of three reported errors

We test the full transit-mask width needed when all mask centers follow one constant period. We use 105,236 published Holczer catalog timings for 1,096 planets marked confirmed in a frozen Kepler DR25 table. Event numbers and each planet's source total duration D stay fixed. Both epoch and period are free. Each true center may move by up to three reported errors from its measured time. A linear program finds the smallest compatible full width. This gives a lower bound on the width for the unknown true centers if all stated bounds hold. For 23 planets, this limit exceeds 1.5D. For 15 planets, it still exceeds 1.5D after any two selected events are removed. A separate control allows for printed-digit rounding in the times and errors. It leaves 22 planets above the width threshold and the same 15 after any two removals. Kepler-9 b has the largest limit, 5.1928D or 22.2757 hours; its limit after any two removals is 5.0861D. Three-event checks cancel epoch and period and prove each positive optimum. An exact branch search tests event removal. We provide the selected measurements, source hashes, code, checks, figures, and per-planet limits. The timing changes are known from prior work. The new result is a catalog of width limits with short proofs. These conditional bounds do not give simultaneous confidence levels, flux losses, detection probabilities, or new planet claims.

Kepler · transit timing variations · transit masks · linear programming · bounded errors · reproducible catalog · event removal

Admitted 1 citing publication

References

10
  1. usesdoi:10.3847/0067-0049/225/1/9

    This work measured the Kepler transit times, errors, source flags, durations, and signal-to-noise ratios used here. We derive new conditional mask-width limits from these published measurements.

  2. usesdoi:10.26093/cds/vizier.22250009

    This CDS catalog supplies the exact tables and source schema. We save URLs and hashes, selected numerical measurements, and code to recover and parse the source files.

  3. usesFixed masks with width 1.5 sibling transit durations remove over 10% of model transit time for 33 of 1,263 Kepler DR25 planets sci:sha256:7ed9974fc8ab2b0840cc298db89f6f73ee16bf6c5434206ac3d1dc9dd283076a

    We reuse its exact frozen NASA DR25 confirmed table and saved query provenance. Its fixed-clock mask-loss test motivates the 1.5-duration comparison. We instead optimize the clock using measured transit times.

  4. Fits with free sibling event depths retain at least 86.1% of target information in 763 Kepler box models with fixed times and equal independent noise sci:sha256:fc0ef1b325d789964e3f35c8f819b16ee8e31f6641909f137246977ea00424c8

    This study compared masks with sibling-depth fits in fixed-time box models. The present bounds test measured timing intervals with a free epoch and constant period.

  5. Five conditional TOI-1136 c transit fits in TESS sector 75 fall outside masks with a stated full width of 6.54 hours sci:sha256:975f9e384a3d2eacef14106338ac0afa63cce5ab97975287ec7013f7b2b55b49

    This study found five conditional TOI-1136 c transit fits outside old masks. We remove old-clock drift as a possible cause by allowing any epoch and constant period.

  6. usesdoi:10.3847/1538-4365/aab4f9

    This paper describes the DR25 catalog used for confirmed status and a separate duration control.

  7. usesdoi:10.26133/NEA4

    The NASA Exoplanet Archive supplies the frozen DR25 response reused from the cited SCI publication.

  8. doi:10.3847/1538-3881/aa62ad

    This work studied planet-search losses from transit masking. Our timing-based necessary widths measure a different quantity from its detection tests.

  9. doi:10.1093/mnras/staf334

    This study used special windows for large timing variations. The general need for such masks is prior knowledge; our contribution gives optimized width limits and inspectable three-event proofs.

  10. usesdoi:10.1038/s41592-019-0686-2

    The code uses the SciPy optimization interface to solve the linear programs with HiGHS. The package records the exact SciPy version and independent numerical checks.

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