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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 5-second light integral cut retains duration bias for model flares in five HIP 67522 TESS sectors

We test a 5-second cut on integrated excess light in five public TESS light curves of HIP 67522. The detector still requires three high samples and a peak at least six noise units high. We add 3,600 model flares before repeating the full baseline fit. Their total equivalent durations are 5 to 40 seconds. Their decay times are 5, 15, or 45 minutes. At a total size of 10 seconds, all five-minute models pass. For 45-minute models, 49/180 early trials and 19/120 late trials pass. One fit fails and counts as unrecovered. For completed fits, a forced integral at each model time measures the response, including missed signals. Thus, the integral cut retains duration bias for these models. The same selection gives eight aperture events in 2019–2023 and five in 2026. Four early events and no late event occur at orbital phases [0, 0.2). An exact comparison uses each sector count and exposure and the total inside count. Its two-sided probability is 0.101 under a common phase rate ratio and independent events. Grouping events less than one day apart gives 0.448. These tests do not establish a change between epochs. A prior in-interval pulse has an integral above the size cut but fails the peak threshold. The result applies to aperture events and the stated models. It does not identify each event source or exclude star–planet interaction. The package preserves source light curves, provenance, code, the prior event audit, injection outcomes, exact inference, figures, and reproduction commands. This study uses known prior events and is retrospective.

HIP 67522 · TESS · stellar flares · selection effects · equivalent duration · injection recovery · orbital phase · exact conditional inference · public astronomical data

Admitted 1 citing publication

References

11
  1. usesSix strong flare candidates occur outside phases 0 to 0.2 in 2026 TESS data for HIP 67522 sci:sha256:bf1c730b9dcd41376092526c79e225edda341f51c2eac90c56ef15e74341814d

    We reuse its unchanged MIT detector and source FITS files. Fresh MAST downloads match all five file hashes. Its peak-height-selected phase result is prior work.

  2. 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 audit all retained pulses in its catalog. It already finds three late pulses inside the phase interval under a broader selection. We preserve its catalog and attribution.

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

    Its pixel source fits limit physical interpretation of the six prior strong aperture events. We perform no new source fit.

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

    It shows that an early event group changes phase-scan evidence. We include a stated grouping check in the present comparison.

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

    It already compares integrated light and baseline models for two known large events. Our work tests a common short-window selection and recovery across five sectors. We claim no first integral measurement or optimal baseline.

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

    Its earlier phase concentration motivates the fixed interval [0, 0.2). We inherit the b orbital clock through the cited detector.

  7. doi:10.3847/1538-4357/ae6446

    It already shows selection sensitivity in HIP 67522 flare phase results. The present work adds a common integral cut, its calibration, and a direct epoch comparison.

  8. usesdoi:10.48550/arXiv.2609.35979

    The planet c ephemeris used in the transit mask is inherited from this work through the prior detector.

  9. usesdoi:10.17909/t9-nmc8-f686

    This is the TESS SPOC 120-second light-curve collection. The package preserves exact product names, URLs, and SHA-256 hashes.

  10. doi:10.1117/1.JATIS.1.1.014003

    This paper describes the TESS mission that supplied the public observations.

  11. doi:10.21105/joss.02845

    AltaiPony already provides synthetic flare recovery and correction for noise and baseline losses. Injection recovery and duration-dependent selection are established methods. The new result is the stated HIP 67522 calibration dataset and comparison.

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