The primary-to-secondary eclipse interval of AI Phoenicis decreased in the 2018–2026 TESS aperture data
We measured separate eclipse times in eight public TESS light curves of AI Phoenicis. Eight events pass the strict quality and coverage rules. The primary-to-secondary interval in 2026 is about five minutes shorter than in 2018. A local phase comparison gives a decrease of 302.2 seconds. Its estimated noise error is 7.1 seconds under the stated aperture-flux and eclipse models. Other tested aperture fitting choices give decreases from 291.1 to 302.9 seconds. Shared quadratic and cubic clock changes do not explain all eight times under these assumptions. The pipeline-corrected flux has much larger scatter and does not confirm the aperture precision. The early comparison uses the published reference period. The data support a change in relative eclipse phase under these limits. They do not establish its physical cause or a new companion. The package includes all eight source FITS files, archive records, code, event times, figures, extraction checks, and repeat instructions.
AI Phoenicis · TESS · eclipsing binary · eclipse timing · orbital phase · public astronomical data
References
5- usesdoi:10.17909/t9-nmc8-f686
The eight SPOC 120-second light curves are the source data.
- usesdoi:10.1093/mnras/staa1662
The reference orbit geometry and fixed quadratic limb coefficients define the local eclipse model.
- usesdoi:10.1093/mnras/stag1398
The early reference period and epoch define cycle numbers. The source also identifies the Sector 29 background problem.
- usesdoi:10.1051/0004-6361/201628581
This work already proposed the primary and secondary timing comparison for AI Phoenicis. We apply that test to later TESS data.
- usesdoi:10.1086/683602
The installed batman quadratic calculation kernel supplies the blocked stellar flux. An independent numerical integration checks this use.
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