{"paper":{"title":"Hidden oscillations in plain sight: identification of seismically unresolved red-giant asteroseismic binary candidates","license":"http://creativecommons.org/licenses/by/4.0/","headline":"Blended oscillations from two red giants in one Kepler aperture produce asteroseismic masses and radii off by up to factors of three and two.","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Francisca Espinoza-Rojas, Jeong Yun Choi, Saskia Hekker","submitted_at":"2026-04-27T13:45:05Z","abstract_excerpt":"Light curves of oscillating stars provide valuable insights into the stellar interiors. When oscillations from a pair of stars are captured within a single photometric aperture, they can be considered as potential asteroseismic binaries (ABs). If the two stars oscillate at similar frequency ranges, the superpositioned oscillation patterns appear as if from a single star, leading to inaccurate asteroseismic parameters. We investigate seismically unresolved AB candidates consisting of two red-giant stars observed by Kepler. We directly compare the power density spectra (PDSs) of blended and sepa"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We identified 6 seismically unresolved AB candidates whose PDS morphologies change noticeably across light curves extracted with different apertures. ... masses and radii for the 6 AB candidates differ by up to about 3 and 2 times relative to the individual stars, respectively.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That changes in PDS morphology when using different apertures are caused by a second oscillating star rather than other instrumental or analysis effects, and that the selected neighbors within 20 arcsec are the source of the additional signal.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Six red-giant asteroseismic binary candidates show blended oscillations that bias mass and radius estimates by factors of up to three.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Blended oscillations from two red giants in one Kepler aperture produce asteroseismic masses and radii off by up to factors of three and two.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"45b70fc19fff4736402968c955a1e18b32946c41f562fe0152085802c73cf0ed"},"source":{"id":"2604.24476","kind":"arxiv","version":1},"verdict":{"id":"9a35e799-4311-4fe2-8e46-cdb916f90df3","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-08T01:37:22.904691Z","strongest_claim":"We identified 6 seismically unresolved AB candidates whose PDS morphologies change noticeably across light curves extracted with different apertures. ... masses and radii for the 6 AB candidates differ by up to about 3 and 2 times relative to the individual stars, respectively.","one_line_summary":"Six red-giant asteroseismic binary candidates show blended oscillations that bias mass and radius estimates by factors of up to three.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That changes in PDS morphology when using different apertures are caused by a second oscillating star rather than other instrumental or analysis effects, and that the selected neighbors within 20 arcsec are the source of the additional signal.","pith_extraction_headline":"Blended oscillations from two red giants in one Kepler aperture produce asteroseismic masses and radii off by up to factors of three and two."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2604.24476/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"ai_meta_artifact","ran_at":"2026-05-21T06:39:41.420483Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_compliance","ran_at":"2026-05-19T22:03:34.341644Z","status":"completed","version":"1.0.0","findings_count":0}],"snapshot_sha256":"9a9d12d99193114ed3153ae3854866902f1c7d34477852d614b4c6557ede9e6b"},"references":{"count":4,"sample":[{"doi":"","year":2016,"title":"The sensitivity and behaviour of the curvature in the \\'echelle diagram of red-giant stars","work_id":"6fec9368-d0ec-4a0d-8b05-8d1ee00294ae","ref_index":1,"cited_arxiv_id":"2603.16597","is_internal_anchor":true},{"doi":"","year":2014,"title":"Mid- dle: combined TPF, with the two custom apertures overplotted in the same colors as corresponding stars","work_id":"d3ce331f-43af-4717-85da-55fc754af86c","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2025,"title":"for KIC 3122188 (TIC 137816135, where TIC is the TESS input catalog) with a cadence of 10 minutes in Sector 40, 41 and 54 (see Fig C.1(d)), and did not detect any oscillation signals higher than the N","work_id":"6faf5555-05a9-4a30-a127-ed894edf3965","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2019,"title":"KEP-A/B\" columns present the results from the PDSs of KEPSEISMIC light curves for ABi-A/B (i=1-6), respectively. The","work_id":"06b655d8-4956-4a25-9a3c-d5d1ee5dba7d","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":4,"snapshot_sha256":"f35773461d9a8928bf94eaef6f9680bec3e56d88b73bb4902734197bbfe7d34e","internal_anchors":1},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}