Archival eclipses support a close stellar companion of TYC 6355-1082-1

Archival eclipses support a close stellar companion of TYC 6355-1082-1 Friedrich Otto KroneIndependent researcher, GermanyORCID: https://orcid.org/0009-0009-5733-2966Observational analysis: 11 October 2026; publication preparation: 16 October 2026 TYC 6355-1082-1, TIC 415683911, Gaia DR3 6832597767349625984 is a previouslycatalogued star. Three independent observing programmes, TESS, SuperWASP and ZTF,show alternating primary and secondary eclipses. Their different depths supporta full orbital period near 5.0151 days, rather than the half-period alias. A closestellar binary interpretation is strongly supported, but worldwide priority anda dynamical companion mass are not established. Gaia DR3 epoch-2016 coordinates are RA 318.91450486442096 degrees andDec -20.233344363000175 degrees; G = 12.0242 mag. The parallax is2.56574 +/- 0.02262 mas. TESS sector 92 contains 9,942 quality-selected QLPmeasurements and four fully covered primary and secondary eclipses. Depths areapproximately 5.80 and 3.87 percent; full durations are near 2.95 and 2.93 hours.TARS re-reduction of the same TESS photons is a sensitivity check, not anotherinstrument. Its independently published rotation catalogue already includesthis known variable at 5.2626 days; that value is not the eclipse orbital period. SuperWASP provides 10,099 original observations, of which 8,763 pass thedocumented selection. Its independently fitted period is 5.0151748 +/-0.0000301 days, with formal errors. Corrected and uncorrected series reproducethe eclipse morphology; FLAG 32 denotes TAMUZ correction rather than a genericbad-quality flag. The ZTF-only fit gives 5.0150754 +/- 0.0000262 days, with formalerrors. A joint constant-period descriptive fit gives 5.0150987 days and primaryepoch BJD_TDB 2460805.517458. Its nominal precision excludes correlated errorsand model uncertainty and is not a guarantee of long-term phase prediction. Primary and secondary TESS difference-image centres lie 0.114 and 0.120 pixelsfrom the target's catalogue position. Bootstrap statistics do not include fullWCS/PSF systematics; these offsets do not prove subarcsecond localization.Known Gaia neighbours are too faint to explain the entire optical light loss.An unresolved multiple-star configuration is not universally excluded.Gaia independently reports 30 RV transits over 886.7 days and a robust full RVrange of 134.42 km/s. Public individual RVs and a phase-resolved spectroscopicorbit were not located; no orbital RV semiamplitude or dynamical mass is claimed. NEOWISE gives additional sparse phase-dependent support. ASAS, NSVS, Catalina,DASCH, APPLAUSE, AllWISE and Pan-STARRS have weak or inadequate eclipse coverageand are not counted as secure extra confirmations. The German six-page reportdocuments those negative and unavailable tests, timing conventions and limits.The model of two luminous spheres is descriptive and does not uniquely determinecomponent radii or temperatures for the grazing eclipses. Earlier searches covered source-linked SIMBAD information, positional VSX andTESS-EB queries, Gaia/SB9/WDS, ExoFOP, 110 VizieR catalogues, the full SchancheSuperWASP table, the Liu et al. 2026 TESS-EB table and Penev 2026 data/code tables.They found no prior matching close-binary interpretation. The recorded 14 October 2026 VSXquery also returns no objects in a 2-arcminute cone around the target. These arefinite searches and cannot prove worldwide priority. The new contribution isthe supported eclipsing-binary interpretation and full period of a known star,not the first observation of the star or the first detection of variability. Data and code: the curated package preserves the original measurements,exposure/cadence time corrections, source and neighbour checks, known-objecttests, analysis scripts, original provenance links and a SHA-256 inventory.The source archive's per-file hashes were verified before repackaging. This isarchive-integrity verification; no fresh independent re-execution of all thehistorical analyses is claimed in this packaging step. Data producers retain attribution and their original terms: NASA TESS/MAST,MIT QLP, TARS, the WASP consortium/CERIT-SC, ZTF/IRSA, ESA Gaia/DPAC, ASAS,NSVS, Catalina, DASCH, APPLAUSE, Pan-STARRS, CDS and AAVSO. Third-party journalPDFs and full journal article texts are excluded. Original observations werenot acquired by the analysing author. Author-created text and analysis codeare offered under CC BY 4.0; this does not override upstream data/code terms.OpenAI Codex assisted data retrieval, analysis code, verification, plots anddrafting. No synthetic astronomical observations were generated. The humanauthor is responsible for the scientific content. Selected primary referenceshttps://archive.stsci.edu/hlsp/qlphttps://archive.stsci.edu/hlsp/tarshttps://zenodo.org/records/19917941https://doi.org/10.1051/0004-6361/201015655https://exoplanetarchive.ipac.caltech.edu/docs/SuperWASPProcessing.htmlhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/488/4905https://www.cosmos.esa.int/web/gaia/dr3https://arxiv.org/abs/2206.05902https://content.cld.iop.org/journals/0067-0049/285/1/5/revision1/apjsae6eeet2_mrt.txthttps://zenodo.org/records/23045396 Archive packaging: The original verified evidence ZIP is distributed byte for byte in 11 small standard ZIP parts because the single large-file transfer failed. Download all TYC6355_Evidence_part_*.zip files, TYC6355_ARCHIVE_MANIFEST.json, TYC6355_RESTORE_ARCHIVE.py and the restoration README. The standard-library Python helper restores the original ZIP and verifies each segment, the full SHA-256, CRCs and all 192 archive members. The full round trip was verified before publication. Original archive SHA-256: 193505eaf926c46247d859bfea5c79ab687707288140f94038b4779c458c0b8e.