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

Linear pointing terms shift the fitted TOI-125 Sector 69 source offset by 1.06 pixels

We test the pixel source positions of three public TESS events linked by earlier SCI work to a 49.06-day sequence at TOI-125. We fit official pixel response models to the local stellar image and the lost-light image. For the Sector 69 event, adding linear pointing terms shifts the relative source position by 1.06 pixels. The aperture depth changes by only 1.35 parts per million. This comparison holds a 0.45-day window half-width, a linear time baseline, a 5 by 5 pixel region, and the event template fixed. We compare 61 model choices per event and use eight nearby transits of known planet b as controls. The fitted source positions depend on the time model. The source remains unresolved, and this test does not confirm or reject an extra planet. We preserve native public pixel subsets, source hashes, response files, code, fitted images, controls, residual-noise tests, figures, and reproduction instructions.

TOI-125 · TIC 52368076 · TESS · difference image · source position · pointing · pixel response function · TOI-125.04 · planet candidate · public data · model sensitivity

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References

11
  1. usesThree TESS events at TOI-125 fit a 49.06-day repeat period under a constant-period model sci:sha256:2f9fc0769d7061399bd32b085cda0004ef833d011fcc999fda64743271448c81

    We use its three TOI-125 event centers and durations. We add numerical source fits, model tests, and known-planet controls to its unresolved image checks.

  2. usesPixel fits place the TOI-2300.03 lost light within 0.13 pixel of the target image in TESS Sector 40 sci:sha256:797d7deacc9d3040695b7273501b89db1515ecd8f291a1bf78cdda601979290f

    We use its source-testing workflow as a method reference. We copy the unchanged Keaton Bell response reader and its MIT notice from its package. All TOI-125 fits and analysis code are new.

  3. usesdoi:10.1086/671767

    We use the difference-image method and compare the lost-light position with the local stellar-image position.

  4. usesdoi:10.48550/arXiv.2609.35607

    Median periods and epochs in Table 3 of version 1 select the known-planet transits. Local timing fits set masks and control templates.

  5. usesdoi:10.17909/t9-yk4w-zc73

    We use the public SPOC target pixel products for TIC 52368076 in Sectors 2, 69, and 96. Native subsets, full-product hashes, addresses, and retained row indices are preserved.

  6. usesdoi:10.17909/t9-nmc8-f686

    We use three public SPOC light curves to fit local times and durations of known-planet controls and masks.

  7. doi:10.1117/12.2233418

    This paper describes the SPOC data pipeline.

  8. usesdoi:10.1051/0004-6361/202243940

    Gaia DR3 positions and proper motions map the target and resolved field stars onto each stamp.

  9. usesdoi:10.26134/ExoFOP5

    The saved ExoFOP rows identify the current period-zero TOI-125.04 entry, which differs from the old short-period signal with that number.

  10. doi:10.3847/1538-3881/ab3f2b

    The first system report defines the old TOI-125 candidate numbers.

  11. doi:10.1093/mnras/staa197

    Prior work measured the masses of the three known planets.

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