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astro-ph.SR · Solar and Stellar Astrophysics

Symmetric fits to five TESS visits of HS 0705+6700 show no resolved common timing curvature from 2019 to 2024

HS 0705+6700 has disputed models of bodies that orbit its eclipsing binary. We measure primary and secondary eclipse clocks in five public TESS visits from December 2019 to January 2024. The main fit uses 120 s SAP flux, an even spline integrated over each exposure, and local flux baselines. It contains 1016 primary events and 1019 secondary events. We compare each middle visit with the line through the first and last visits. The common departures are 1.09 ± 1.11 s in sector 47, 0.46 ± 0.91 s in sector 60, and 0.12 ± 1.38 s in sector 73. Errors use paired one-day noise blocks. Full two-day block deletion gives larger common-component errors of 1.56 s, 1.23 s, and 1.76 s. No tested flux, cadence, knot, baseline, or window choice gives a common departure above two estimated one-day errors. A wider window with a linear baseline gives a weak 6.00 ± 2.34 s secondary-minus-primary departure in sector 60. It falls to 1.85 ± 3.04 s with a cubic baseline in the same window. The difference signal therefore depends on the flux baseline. The package gives paired event centers, covariance matrices, source hashes, input columns, code, and reproduction commands. These measurements assume symmetric eclipse flux. They do not identify a planet or exclude timing changes in the gaps.

HS 0705+6700 · V470 Cam · TESS · eclipsing binaries · eclipse timing · secondary eclipse · public data

Admitted 2 citing publications

References

9
  1. usesdoi:10.17909/T9-NMC8-F686

    The five 120 s SAP and PDCSAP light curves are the main public input data.

  2. usesdoi:10.17909/T9-ST5G-3177

    Four 20 s light curves supply a cadence check. They share exposures with the 120 s data.

  3. usesdoi:10.1093/mnras/staf1636

    Equation 1 supplies a reference clock for the eclipse windows. Our contrasts restore its quadratic term and remove its constant and linear terms.

  4. doi:10.1017/pasa.2024.50

    This prior work measured primary TESS eclipses in sectors 20, 47, and 60 and tested companion models.

  5. doi:10.1051/0004-6361/201118105

    This prior work used primary and secondary eclipses of HS 0705+6700 to test orbital rotation.

  6. doi:10.31577/caosp.2024.54.2.228

    This prior primary-eclipse TESS survey included HS 0705+6700 and discussed time sampling and stellar flux errors.

  7. usesSymmetric eclipse fits show a shared 18 s departure in NY Vir TESS sector 91 from the line through sectors 23 and 50 sci:sha256:27b21c0322f367cb77dd5de188a0263813889acfbe0c8c05fdf1771a37dae920

    We use the related paired timing contrast from the line through end visits on a different target. The present code was written independently.

  8. usesLinear and cubic flux baselines give HW Vir secondary eclipse delays that differ by 0.23 seconds in 2016 K2 SAP data sci:sha256:a34346465621bef51c2411f46a2d201049a1e339d62bf7e4b7ade558c055c573

    We use related even spline fits, exposure integration, and local baseline checks on a different target. The present code was written independently.

  9. Symmetric TESS fits give a 2022 to 2024 interval 28 seconds longer than the 2025 quadratic clock for NSVS 14256825 sci:sha256:2c0f59e955f8f27dd1f8a855590204c65f47947b7a46db99d359c1e2941edbe1

    This related work used paired TESS timing measurements for another binary after a shared envelope phase.

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