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

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

We test how a pulse trigger changes a fixed orbital-phase count for HIP 67522. We use public 120-second TESS light curves from sectors 101 and 102. With a measured peak cut of 0.3%, three consecutive high samples select seven aperture candidates. All seven lie outside planet b phases 0 to 0.2. Two consecutive high samples select eleven candidates, with three inside. The prepared arrays, noise scale, masks, peak cut, and merge rule stay fixed. Two added inside peaks match earlier catalog peaks exactly. A third added pair peaks 16 minutes after the earlier listed peak. The 0.5% sample stays at three candidates, all outside. A conditional independent-event model gives central 95% intervals for the selected inside/outside rate ratio of 0 to 2.75 for seven candidates and 0.26 to 6.50 for eleven. Neither lower-cut rule shows a significant excess under equal rates. We add 9,000 model pulses and compare both rules on each identical refitted light curve. For true 0.5% peaks at the 0.3% measured cut, recovery rises from 1,244 to 1,632 of 1,800 trials. The trial grid preserves phase groups. It does not define a physical flare population. Earlier work already identified the same events and selection concerns. The added contribution is this controlled trigger audit and paired response dataset. The relaxed sample is automatic. It is not a validated flare catalog. The results do not confirm each event source or test all star-planet interaction models. The package includes original data, provenance, unchanged frozen files, code, trial records, figures, and offline reproduction steps.

HIP 67522 · TESS · stellar flares · trigger selection · injection recovery · orbital phase · reproducible research

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References

13
  1. usesThree of twelve selected HIP 67522 aperture pulses occur at orbital phases 0 to 0.2 in TESS sectors 101 and 102 sci:sha256:d5bbf5d78aab33fdbbc0ac87b7c3bd553e250e01c0e95aab6aa9a2c7e34d311c

    We use its retained pulse tables for the peak and trigger audit. This work already identified three inside pulses in the same sectors.

  2. usesSix strong flare candidates occur outside phases 0 to 0.2 in 2026 TESS data for HIP 67522 sci:sha256:bf1c730b9dcd41376092526c79e225edda341f51c2eac90c56ef15e74341814d

    We preserve its strong-event table as a comparison input. It already tested six strong 2026 candidates.

  3. usesA 5-second light integral cut retains duration bias for model flares in five HIP 67522 TESS sectors sci:sha256:86cfdd4cc6ea6675eca24985a0ee3a3f4e4d5263ef092f9e5a2511149c133769

    We preserve its prior-catalog audit table for method context. It already measured duration bias under another detector.

  4. TESS PRF fits place two of six fixed 2026 events within 3 arcsec of HIP 67522 for all 18 baselines sci:sha256:c17bc309448383bdf6f39cbbc2284da0ab4b506f26ba776b89d4b400bad9c364

    This source study limits physical interpretation of the shared aperture events.

  5. Two rotation harmonics give the lowest gap prediction error among 13 models in two HIP 67522 TESS sectors sci:sha256:15208568fb23c4bd0c9239cff8a4b797eb44b42dffca100651cd0ca345c2cb18

    This prior study measures how the baseline affects integrated light for two known events.

  6. One fixed group raises the orbital scan tail for the 12 TESS flares of HIP 67522 sci:sha256:3660abd9a8c2e7591ae0a20fb434419aafc2bed8b585d67306af0e9f8714b5b6

    This prior study tests temporal groups in the earlier flare phase scan.

  7. usesdoi:10.1038/s41586-025-09236-z

    The reported phase interval sets the present test question. Its energy-selected sample differs from our peak-selected candidates.

  8. doi:10.3847/1538-4357/ae6446

    This paper already tests selection effects in the earlier HIP 67522 flare sample.

  9. usesdoi:10.48550/arXiv.2407.04763

    Version 2 gives the adopted planet b period and transit reference.

  10. usesdoi:10.48550/arXiv.2609.35979

    James et al., version 1, Table 3 gives the c transit mask and the updated b clock.

  11. usesdoi:10.17909/t9-nmc8-f686

    This MAST collection supplies the five original 120-second SPOC light curves. Product names and hashes define the subset.

  12. usesdoi:10.17909/t9-st5g-3177

    This MAST collection supplies the two original 20-second SPOC light curves for display checks.

  13. doi:10.21105/joss.02845

    AltaiPony provides established methods for model injection and recovery in flare analysis.

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