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

A Gaia binary candidate gives the best catalogue fit to the fixed 4.554-day TOI-1216 dip in 10 of 12 models

We tested the source of the known broad dip assigned to TOI-1216.01. We used 43 public TESS target pixel products and held the earlier 4.554183-day period and 10.098-hour shape fixed. Four local baseline models retain 198 events. Their mean SPOC aperture depths range from 183 to 252 parts per million. The primary depth rises from 159 to 250 parts per million between 3 by 3 and 7 by 7 pixel apertures. We compared 28 Gaia sources with G<20 within 100 arcseconds. Gaia DR3 4648442077964982912 is an eclipsing-binary candidate 31.43 arcseconds from the target. It gives the lowest catalogue source score in 10 of 12 model cases. The nearest star wins the other two; the target wins none. All nine free-position fits with time or spatial motion terms lie within 1.3 arcseconds of the binary candidate's catalogue offset. These fits reuse the same data and have no calibrated position errors. Fits without motion terms give other positions. Six control phases have mean depth intervals that include zero. In the spatial derivative model, injections at the binary candidate favour it over the target at five of six phases. These injections have a depth of 200 parts per million. The same response model makes and fits the injections. Controls without spatial derivatives show large source-score artifacts. Scores use formal pixel errors, and amplitudes have no cap from stellar flux. The Gaia orbital period is 0.756240 days; six times that period differs from the tested TESS period. This work identifies a conditional source candidate. It does not establish the cause of the dip or confirm a planet. The package preserves reduced pixels, input hashes, code, loss images, tables, figures, controls, and reproduction instructions.

TOI-1216.01 · TIC 141527965 · TESS · source position · difference images · aperture photometry · exoplanet candidates

Admitted 3 citing publications

References

11
  1. usesFolded TESS PDC light curves retain broad dips in four of five selected duration anomalies sci:sha256:cf43edf807bbed7e03cbdd1dc4c4e9f5e141cd3daa392e051f2bfb6053d44628

    This publication supplies the selected target, all 43 light-curve inputs, and the fixed broad dip model. We reuse its observations for pixel source tests.

  2. usesTESS pixel fits in 23 sectors link TOI-785.01 to the known binary OGLE-LMC-ECL-38842 sci:sha256:50b019bef9a061a6ab722f5edef282b842173a3df0326924f4bf4b9e45d68a95

    Pixel reduction and TESS response model code were adapted from this study of another target. Its MIT notice is retained.

  3. Nine later TESS sectors give a positive mean depth for a fixed transit model of TOI-1216.01 sci:sha256:cdee96756caba9d3a3eabc142db8d08fbdd96f0c086ba4c579fb9a669b1589c9

    This earlier study tests the same target in nine later TESS light-curve sectors. It does not identify the source with pixel loss images.

  4. Two models from earlier data give positive fitted depths for TOI-1216.01 in TESS sectors 88–98 sci:sha256:1c8e86a828aee64195b716dfd88ec03157fcb8cdac3227821e59aecf8925a048

    This earlier light-curve study tests two fixed models for the same target and shows a dependence on the dip width.

  5. doi:10.1093/mnras/stab1167

    This study reports that the TOI-1216 transit signal was too weak for its fits.

  6. doi:10.3847/1538-3881/abc6af

    Table 7 gives the earlier TRICERATOPS result for this candidate. The present work does not update those probabilities.

  7. doi:10.3847/1538-3881/ac17f6

    Table 7 supplies the 2019 SOAR target row and its finite companion detection limits.

  8. doi:10.1086/671767

    This paper describes source tests with difference images and centroids in public transit data.

  9. usesdoi:10.1051/0004-6361/202243940

    Gaia DR3 supplies the field catalogue, proper motions, and selected variability records.

  10. doi:10.1117/12.2233418

    This paper describes SPOC, which produced the public calibrated TESS inputs.

  11. usesdoi:10.1051/0004-6361/202245330

    This paper describes the Gaia DR3 eclipsing-binary candidate table and its orbital frequency. We use the saved field source record as a source candidate, not as a confirmed cause of the TESS dip.

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