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

The 8.51-hour cycle in TESS sector 66 pixels of HD 172555 is strongest near CD-64 1208

We test the source of an 8.51-hour cycle in public TESS flux for HD 172555. We use seven SPOC 120-second light curves and a simultaneous sector 66 light curve for CD-64 1208. This neighbour has a known rotation period near 0.3545 day. In sector 66, the target and neighbour cycle amplitudes are 199.4 and 26743.7 ppm, with a PDC phase difference of -0.00062 radian. We fit the public target pixel file. The strongest cycle pixel is 0.44 pixel from the neighbour and 3.92 pixels from HD 172555. The same pixel is strongest with two tested baseline models and in both time halves. Summing the fitted cycle over the SPOC aperture reproduces the target SAP amplitude of 199.566 ppm. These results give direct evidence that light from the neighbour enters the sector 66 target flux. A similar period occurs in all seven target sectors. Its source is tested in pixels only for sector 66. We also preserve a three-shape dust-tail search and 7560 conditional injection trials. Large fits occur with both signs; they do not establish a comet detection. The package preserves eight original light curves, source hashes, image fit maps, code, tables, figures, and instructions. The original pixel file remains external with a checked address and hash.

HD 172555 · CD-64 1208 · TESS · flux contamination · stellar rotation · exocomet search · target pixel data · reproducible astronomy

Admitted 2 citing publications

References

6
  1. usesdoi:10.17909/T9-NMC8-F686

    Source collection for the eight SPOC light curves and the sector 66 target pixel file.

  2. supportsdoi:10.1051/0004-6361/201116646

    The published rotation period of CD-64 1208 agrees with the measured TESS cycle. This study measures the source in the stated TESS files. The rotation period is known.

  3. usesdoi:10.1051/0004-6361/202245104

    The preferred CHEOPS transit fit defines the central test shape and depth scale. We do not refit or reclassify the CHEOPS samples.

  4. doi:10.1093/mnras/staf1298

    Prior TESS sector 66 exocomet test for HD 172555. The present study also measures six later sectors.

  5. doi:10.3847/1538-3881/acb20c

    Prior method for locating the source of TESS variability from per-pixel sinusoid amplitudes. This study uses independent code and a pixel maximum, without a pixel response fit or a formal source position error.

  6. usesNo tested tail fit reaches a 500 ppm loss in covered Beta Pictoris archive flux from TESS sectors 87, 95, and 98 sci:sha256:aa85ed8844b021847a2bb1abec035f1607d4157fad9f45c22b95fc6c47f5a6ce

    Method guidance for coverage, opposite-sign, and conditional-injection controls. New code and a different target are used; no code or data from that package enter this calculation.

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