{"paper":{"title":"Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Dynamically formed eccentric stellar-mass black hole binaries produce a detectable population for LISA in the Milky Way and at cosmological distances.","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Bence Kocsis, Erez Michaely, Kyle Kremer, Michael L. Katz, Smadar Naoz, Zeyuan Xuan","submitted_at":"2026-05-14T18:00:00Z","abstract_excerpt":"Eccentric binary black holes (BBHs) formed through dynamical interactions can significantly contribute to gravitational wave (GW) detections. In this work, we present a simulated catalog of dynamically-formed, stellar-mass BBHs in the local universe, incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters (N-body interactions). Our results predict a wide, highly eccentric BBH population in the Milky Way (MW), with source counts of $\\sim 36, 13, 4.7, 2.3, 1.0$ (for $\\mathrm{SNR} > 1, 3, 8, 20, 50$, respe"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"Our results predict a wide, highly eccentric BBH population in the Milky Way (MW), with source counts of ∼36, 13, 4.7, 2.3, 1.0 (for SNR > 1, 3, 8, 20, 50, respectively) during a 10-yr LISA observation. ... our model yields a merger rate of Γ ∼ 9 Gpc^{-3} yr^{-1} and ∼490 extragalactic mHz BBHs with SNR > 1.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The simulated catalog accurately captures the full population by incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters (N-body interactions) as the dominant formation channels for eccentric stellar-mass BBHs.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Simulations of dynamically formed eccentric stellar-mass BBHs predict dozens of LISA-detectable sources in the Milky Way, hundreds of low-SNR extragalactic mHz sources, a merger rate of ~9 Gpc^{-3} yr^{-1}, and potential biases in LISA global fits.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Dynamically formed eccentric stellar-mass black hole binaries produce a detectable population for LISA in the Milky Way and at cosmological distances.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"5fadde2074b4f4bb16b56b03339efddf9f3d054f343ddef1965a43abad1825ce"},"source":{"id":"2605.15265","kind":"arxiv","version":1},"verdict":{"id":"46bf2687-5f66-4fff-ab69-3674c7f54654","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T16:13:47.611916Z","strongest_claim":"Our results predict a wide, highly eccentric BBH population in the Milky Way (MW), with source counts of ∼36, 13, 4.7, 2.3, 1.0 (for SNR > 1, 3, 8, 20, 50, respectively) during a 10-yr LISA observation. ... our model yields a merger rate of Γ ∼ 9 Gpc^{-3} yr^{-1} and ∼490 extragalactic mHz BBHs with SNR > 1.","one_line_summary":"Simulations of dynamically formed eccentric stellar-mass BBHs predict dozens of LISA-detectable sources in the Milky Way, hundreds of low-SNR extragalactic mHz sources, a merger rate of ~9 Gpc^{-3} yr^{-1}, and potential biases in LISA global fits.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The simulated catalog accurately captures the full population by incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters (N-body interactions) as the dominant formation channels for eccentric stellar-mass BBHs.","pith_extraction_headline":"Dynamically formed eccentric stellar-mass black hole binaries produce a detectable population for LISA in the Milky Way and at cosmological distances."},"integrity":{"clean":false,"summary":{"advisory":1,"critical":0,"by_detector":{"doi_compliance":{"total":1,"advisory":1,"critical":0,"informational":0}},"informational":0},"endpoint":"/pith/2605.15265/integrity.json","findings":[{"note":"DOI in the printed bibliography is fragmented by whitespace or line breaks. A longer candidate (10.1103/phys-revd.99.123025) was visible in the surrounding text but could not be confirmed against doi.org as printed.","detector":"doi_compliance","severity":"advisory","ref_index":116,"audited_at":"2026-05-19T16:27:10.328921Z","detected_doi":"10.1103/phys-revd.99.123025","finding_type":"recoverable_identifier","verdict_class":"incontrovertible","detected_arxiv_id":null}],"available":true,"detectors_run":[{"name":"doi_title_agreement","ran_at":"2026-05-19T16:31:18.390629Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_compliance","ran_at":"2026-05-19T16:27:10.328921Z","status":"completed","version":"1.0.0","findings_count":1},{"name":"claim_evidence","ran_at":"2026-05-19T14:41:54.272973Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"ai_meta_artifact","ran_at":"2026-05-19T13:33:22.808924Z","status":"skipped","version":"1.0.0","findings_count":0}],"snapshot_sha256":"947463e72b890c3ac2b2bee5604a27d93d961d284464f4be2f165ed5e5c0132f"},"references":{"count":121,"sample":[{"doi":"10.1103/physrevlett.116.061102","year":2016,"title":"B. Abbott, R. Abbott, T. Abbott,et al., Physi- cal Review Letters116, 10.1103/physrevlett.116.061102 (2016)","work_id":"e55fd158-3b61-42c3-8e7b-2564a9a72dd0","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2021,"title":"The population of merging compact binaries inferred using gravitational waves through GWTC-3","work_id":"04e0474f-c87d-48a4-a278-08f533322b30","ref_index":2,"cited_arxiv_id":"2111.03634","is_internal_anchor":true},{"doi":"","year":2023,"title":"R. Abbott, T. D. Abbott, F. Acernese,et al.(LIGO Scientific Collaboration, Virgo Collaboration, and KA- GRA Collaboration), Phys. Rev. X13, 041039 (2023)","work_id":"a6093905-2764-488e-8773-fb882f78e403","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1007/s41114-022-","year":2023,"title":"P. Amaro-Seoane, J. Andrews, M. Arca Sedda,et al., Living Reviews in Relativity26, 10.1007/s41114-022- 00041-y (2023)","work_id":"8b5e5d7b-bf13-4091-9b09-9f956687c3d7","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2016,"title":"Luoet al.(TianQin), TianQin: a space-borne gravitational wave detector, Classical Quantum Gravity33, 035010 (2016), arXiv:1512.02076 [astro-ph.IM]","work_id":"6938d8d9-beb8-4a5e-ad7e-06e38d30620d","ref_index":5,"cited_arxiv_id":"1512.02076","is_internal_anchor":true}],"resolved_work":121,"snapshot_sha256":"2defc9a5000e6fbe54b04408d9af3c898ed2c18f3789e63753dd4ac19e3160cc","internal_anchors":40},"formal_canon":{"evidence_count":2,"snapshot_sha256":"45e3c64646e1a1693112fd9de013ddfa140c2d9cdb24065eb44f5750ea49824c"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}