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

A Gaia binary candidate near TOI-1546.01 has a compatible catalog period and eclipse time

We tested whether a nearby binary can supply the dips assigned to the planet candidate TOI-1546.01, or TIC 194203348. Gaia DR3 source 384251315018012800 lies 10.81 arcseconds from the assigned star. Its converted period is 1.132825690 days. The TOI and Gaia periods differ by 1.04 combined standard errors. Their primary times differ by 19.35 minutes and agree within an approximate propagated error. At the fixed Gaia period, 18 events in TESS sector 17 give a dip of 476 +/- 107 parts per million. QLP extractions of the same exposures also contain the dip. Image fits give weak source evidence that changes with the model. The main weighted residual sums are 58.87 at the assigned star and 56.18 at the binary. A whole-event bootstrap includes both positions. A model with independent spacecraft pointing terms reverses the small residual preference. A phase-0.25 brightening also limits the baseline model. The sector 84 cutout is on calibration columns and gives no second source test. The binary remains a possible source, but these data do not establish a false positive or a new planet. Existing ExoFOP follow-up reports were not accessible. We supply the input data, queries, hashes, code, results, figures, and offline reproduction instructions.

TESS · TOI-1546.01 · TIC 194203348 · Gaia DR3 · eclipsing binaries · source location · transit dilution · catalog match · reproducible astronomy

Admitted 1 citing publication

References

9
  1. usesdoi:10.1051/0004-6361/202245330

    Gaia binary records supply the known binary identity, frequency, eclipse phase, and model errors.

  2. usesdoi:10.5270/esa-qa4lep3

    Gaia DR3 supplies positions, proper motions, magnitudes, and the eclipsing-binary row.

  3. doi:10.3847/1538-4365/abefe1

    This paper describes the TOI catalog. Current values come from the archived NASA Exoplanet Archive response.

  4. usesdoi:10.17909/t9-r086-e880

    We fit the archived sector 17 QLP version 01 aperture products. They use the same TESS exposures as the cutout.

  5. doi:10.3847/1538-3881/acb20c

    This paper describes established PRF fits to TESS variable-source images.

  6. usesFixed TESS models give lower residual sums at Gaia binary positions than at the assigned stars for two TOIs in four sectors sci:sha256:d47c589177bbec84c6559fc996322eb3b55cbb22309d9277422afb3ac8940494

    We use the pairwise fixed-position image test design for a different field. We write new analysis code and do not claim a new method.

  7. usesCatalog light loss estimates agree within a factor of 1.2 for 41 of 50 TOI pairs matched near BJD 2460000 sci:sha256:c649ef53d8c7493c75c894ce7b14411564d02c45946456d238999a95f1cf6979

    The preserved ExoFOP table supplies the context row and the count of existing follow-up observations. It does not enter a numerical fit.

  8. usesdoi:10.26134/ExoFOP5

    The cited SCI snapshot preserves the ExoFOP TOI table. Individual follow-up reports were inaccessible and were not reviewed.

  9. doi:10.1117/1.JATIS.1.1.014003

    This paper describes the TESS mission, whose public images support this case study.

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