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TESS fits show eclipse phase offsets above 0.20 in six tested catalog entries with periods from 2 to 5 days

We tested nine entries in the TESS Ten Thousand catalog. We selected all entries with periods from 2 to 5 days and catalog eclipse phase offsets above 0.20. Fits to 16 archived TESS series show large offsets in six entries. These results pass changes to the local baseline, eclipse shape, flux extraction, and period bound. We estimated uncertainty by removing one orbital cycle at a time. The phase ranges, with the measured uncertainty added, stay above the selected offset threshold in the six representative series. TIC 127140421 has a measured second eclipse phase of 0.78674, with a conditional 95 percent interval from 0.78616 to 0.78732. An exact timing relation gives an eccentricity above 0.46 at its sensitivity envelope, if the eclipses form one central pair in an edge-on Kepler orbit at the adopted period. TIC 265749614 gives a further pair after additive baseline correction, but its interval crosses the selected threshold. Two other entries remain unresolved. This work supplies new phase measurements and a reproducible audit. It does not establish new planets or new binary discoveries. The package includes frozen data, source hashes, code, failed fits, tables, and figures.

TESS · eclipsing binaries · eccentricity · eclipse timing · public data · reproducible astronomy

Admitted 2 citing publications

References

10
  1. usesTESS fits place secondary eclipses near phase 0.5 in three selected TESS Ten Thousand entries with periods of 1 to 2 days sci:sha256:973140eeeb81d1928dd2af43de054a2be0590536c49fbd67ac005a1f10f2b139

    We adapt its MIT eclipse fitting code and extend the audit to nine different entries with periods from 2 to 5 days.

  2. usesdoi:10.3847/1538-4365/ade2d8

    This catalog paper defines the source sample and already reports the candidate eclipse pairs.

  3. usesdoi:10.26093/cds/vizier/bb-8q-1j

    We use Table 3 and preserve the source table and its field definitions.

  4. usesdoi:10.17909/t9-r086-e880

    We use archived QLP light curves.

  5. usesdoi:10.3847/2515-5172/abca2e

    This paper describes QLP light curves from the TESS primary mission.

  6. usesdoi:10.3847/2515-5172/ac2ef0

    This paper describes QLP light curves from the extended mission.

  7. usesdoi:10.17909/610m-9474

    We use archived TGLC light curves.

  8. usesdoi:10.3847/1538-3881/acaaa7

    This paper describes the TGLC flux extraction method.

  9. usesdoi:10.3847/2515-5172/ab1e4a

    We use TESSCut to obtain raw pixel series.

  10. usesdoi:10.1088/2041-8205/763/1/L2

    We use its exact eclipse timing limit to compute conditional minimum eccentricities.

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