Three of twelve selected HIP 67522 aperture pulses occur at orbital phases 0 to 0.2 in TESS sectors 101 and 102
We test a reported excess of HIP 67522 flares near the transit of planet b with later TESS data. Sectors 101 and 102 cover March and April 2026. A local plan set the phase interval and pulse-selection rule before data inspection. It was not registered with a third party. We selected pulses with a measured peak rise of at least 0.3% and three consecutive points above three noise units. We inspected candidate profiles before we calculated orbital phases. We retained twelve of sixteen automated candidates, including three uncertain pulses. All six stronger events in an earlier SCI list are retained. Six additional aperture pulses include all three peaks inside the interval. The physical sources of the aperture pulses remain unconfirmed. The interval is phase at least zero and below 0.2 under the original published orbital clock. Searched time is 8.306 days inside this interval and 31.431 days outside. A conditional count model gives an inside/outside rate ratio of 1.26, with an exact 95% confidence interval of 0.22 to 5.12. The one-sided probability for an excess under equal rates is 0.476. The model assumes independent events and a constant rate within each sector under the null. This selected sample does not show a significant excess in the fixed interval. It differs from the earlier energy-selected sample and does not exclude variable star-planet interaction. The package preserves public light curves, pixel extracts, source hashes, frozen selection decisions, figures, injection trials, and code to repeat the result.
HIP 67522 · TESS · stellar flares · star-planet interaction · orbital phase · selection effects · reproducible research
References
9- usesdoi:10.1038/s41586-025-09236-z
This paper supplies the target, primary orbital clock, fixed phase interval, and earlier result for comparison.
- doi:10.3847/1538-4357/ae6446
The final paper, section 7.6, shows how flare selection affects inference from the older HIP 67522 observations.
- usesdoi:10.48550/arXiv.2606.18045
Version 1 supplies both planets' transit masks and the alternate orbital clock.
- usesdoi:10.17909/t9-nmc8-f686
TESS 120-second light curves from sectors 11, 38, 64, 101, and 102. Exact products and hashes are in the package.
- usesdoi:10.17909/t9-st5g-3177
TESS 20-second light curves from sectors 101 and 102 for pulse-profile checks.
- usesdoi:10.17909/t9-yk4w-zc73
TESS 120-second target-pixel files from sectors 101 and 102 for image checks. Time-window extracts are preserved.
- usesSix strong flare candidates occur outside phases 0 to 0.2 in 2026 TESS data for HIP 67522 sci:sha256:bf1c730b9dcd41376092526c79e225edda341f51c2eac90c56ef15e74341814d
This earlier study tested the same 2026 sectors. Six published event rows supply a reference list for comparison. Our twelve-pulse list retains all six and adds six pulses under a different selection rule.
- 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 gives image-position limits for the six shared events. Our qualitative images do not replace its source tests.
- doi:10.48550/arXiv.2609.35979
Version 1 uses TESS sectors 101 and 102 for transit timing. These observations have been studied before.
Cited by
3 publicationsPublic catalog entries on Sciscape.
- usesTwo rotation harmonics give the lowest gap prediction error among 13 models in two HIP 67522 TESS sectors
Additional pulse times excluded from local baselines; archive URLs used to locate source products.
- usesA 5-second light integral cut retains duration bias for model flares in five HIP 67522 TESS sectors
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.
- usesA 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 use its retained pulse tables for the peak and trigger audit. This work already identified three inside pulses in the same sectors.