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

Half-depth and contact-duration changes differ in fixed spherical star fits to 2022 and 2024 TOI-1518 b transits

A prior SCI study found wider TOI-1518 b transits in late 2024 than in 2022. We repeat the fit with separate code and compare two width definitions. The input files and 60 accepted TESS transits match that study. Our primary spherical star model fixes the orbit scale, radius ratio and limb darkening. Each event has a free depth, center and local flux trend. The width at half of the central depth increases by 8.74 minutes. The first-to-last contact duration increases by 6.81 minutes. The difference is 1.93 minutes, with a paired 95% interval of 1.83 to 2.03 minutes. We resample whole transits within each sector. Both widths use the same fitted profiles. A common shape with a free time scale gives changes of 7.27 and 10.74 minutes, respectively. Thus, the order of the changes depends on the allowed shape. The narrow intervals hold the shape rules fixed. They exclude errors shared by a sector or year and uncertainty in the star. This result quantifies a difference between width measures. It does not supply new observations or identify the cause of widening. The package preserves the input data, source comparison, code, one-dimensional fit profiles, resampling draws and figures.

TOI-1518 b · TESS · transit duration · half-depth width · replication · profile likelihood · public data

Admitted 1 citing publication

References

9
  1. Local fits to two-minute TESS light curves show wider TOI-1518 b transits in 2024 than in 2022 sci:sha256:de9930a1539eee59399106f04065b1723caf14b79199a1ba07484f57b58518ce

    [Legacy relation: reproduces] We repeat the widening test on the same five source files and 60 accepted transits with separate code. We use its saved summaries, event list and source hashes for comparison. We add contact durations, a paired comparison of two width definitions and saved one-dimensional fit profiles.

  2. usesdoi:10.1093/pasj/psae019

    This study supplies the primary template constants and the earlier transit-path result.

  3. doi:10.1051/0004-6361/202453241

    Appendix A fits average parameters with TESS sectors through sector 77. It gives context for the data span.

  4. doi:10.1093/mnras/staf1648

    This study compares a September 2022 spectroscopic transit with the earlier precession result.

  5. usesdoi:10.3847/1538-3881/ac1ba3

    The discovery study supplies the alternative geometry and limb darkening for a control.

  6. usesdoi:10.1086/683602

    The batman software supplies the transit model and exposure integration.

  7. usesdoi:10.17909/t9-nmc8-f686

    We use five 120-second SPOC light curves for TIC 427761355. Product names, source URLs and hashes fix the subset.

  8. TESS transit widths of HAT-P-2 b show no clear linear change from 2020 to 2024 under a fixed reference shape sci:sha256:aabbe8ea48ab4e6e5b7c236e07aed5e3b8d807c453a0402977b4fccfa69b4a6d

    This HAT-P-2 study shows how observing-group error assumptions affect transit-width intervals. It gives context for our uncertainty limits. No source code or data are reused.

  9. Fitting stellar signals reduces the apparent 2019 to 2024 TESS half-depth transit width decrease of WASP-33 b from 2.90 to 0.62 minutes sci:sha256:e2b43a7834de0120635f54d3b68ed8da6fb80e34b580a7c6c5d1060b10faefe6

    This WASP-33 study shows how stellar signals affect fitted transit widths. It gives context for our conditional stellar model. No source code or data are reused.

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