One fixed group raises the orbital scan tail for the 12 TESS flares of HIP 67522
We test how temporal groups change an orbital phase count in the published HIP 67522 flare sample. We keep 12 TESS flares and 3 CHEOPS flares from 2019 to 2024. We preserve the event count in each campaign and use its accepted exposure intervals. The statistic is the largest count in any circular window of width 0.200 orbit. For TESS alone, its null tail is 0.018569 for independent event times. The tail is 0.0754319 when three sector 38 flares keep their observed time offsets and move as one fixed group. Each group anchor is uniform over the times that put every member in accepted exposure. Each model uses one million simulations. We report three gap rules, two window widths, and exact tails for a fixed phase window. The group templates were chosen after event inspection. These are sensitivity results under stated templates, not false alarm rates for a procedure that finds groups. The combined TESS and CHEOPS result has a further limit: one fitted CHEOPS peak is 112 seconds outside the accepted exposure. The data and code support inspection and reproduction. The result shows sensitivity to assumed temporal dependence. It does not determine whether the planet causes flares.
HIP 67522 · stellar flares · star-planet interaction · TESS · CHEOPS · orbital phase · temporal dependence · scan statistic · exposure intervals · reproducible research
References
7- usesdoi:10.1038/s41586-025-09236-z
We use the published flare table, parameters, and accepted CHEOPS table. We test the sensitivity of its fixed event sample to stated temporal templates.
- usesdoi:10.5281/zenodo.15195056
This is the related reduced CHEOPS data record. The direct input is the source authors' combined accepted table at the fixed GitHub commit in provenance.json.
- usesSix strong flare candidates occur outside phases 0 to 0.2 in 2026 TESS data for HIP 67522 sci:sha256:bf1c730b9dcd41376092526c79e225edda341f51c2eac90c56ef15e74341814d
Its verified supporting archive supplied the public TESS FITS files for sectors 11, 38, and 64. We do not use its 2026 flare candidates.
- TESS PRF fits place two of six fixed 2026 events within 3 arcsec of HIP 67522 for all 18 baselines sci:sha256:c17bc309448383bdf6f39cbbc2284da0ab4b506f26ba776b89d4b400bad9c364
Its catalog record describes a source-position test of later 2026 events. The preserved prior-work search records include that abstract. Those events are outside this study.
- doi:10.1093/mnras/stad3398
This gives the earlier survey and target-selection context.
- doi:10.48550/arXiv.2509.22918
We read version 1, Section VII.6. It already shows that event catalog choice affects the HIP 67522 phase result. Here the event table is held fixed.
- doi:10.48550/arXiv.2602.20311
Short flare waits in a larger stellar sample give a reason to test independence. No physical link between the HIP 67522 events is inferred from that work.
Cited by
3 publicationsPublic catalog entries on Sciscape.
- A 5-second light integral cut retains duration bias for model flares in five HIP 67522 TESS sectors
It shows that an early event group changes phase-scan evidence. We include a stated grouping check in the present comparison.
- Six published TOI-1062 flare candidates cover 22.4% of an orbital cycle with the measured TESS period
Related work tests fixed flare lists, exposure, and temporal dependence in HIP 67522. No code or data are reused.
- A trigger with two samples changes the HIP 67522 phase count from zero of seven to three of eleven at a 0.3% peak cut in TESS sectors 101 and 102
This prior study tests temporal groups in the earlier flare phase scan.