{"paper":{"title":"Impact of the axion-like self-interactions in gravitational atoms for LISA","license":"http://creativecommons.org/licenses/by/4.0/","headline":"Axion-like particles forming halos around black holes cause detectable dephasing in LISA waveforms from inspiraling binaries.","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"gr-qc","authors_text":"Carlos Palenzuela Luque, Samuel G\\'omez G\\'omez, Xisco Jimenez Forteza","submitted_at":"2026-05-17T18:33:22Z","abstract_excerpt":"Ultralight bosons with self-interactions, such as axion-like particles, can form astrophysical Bose-Einstein condensates around stars or compact objects, often referred to as gravitational atoms. In this work, we adopt a recently proposed dynamical formation mechanism for these halos and estimate their impact on extreme- and intermediate-mass-ratio inspirals when present around the primary black hole. We show that, for signal-to-noise ratios $\\lesssim 100$, LISA can distinguish gravitational waveforms from binaries embedded in such halo overdensities. Our analysis indicates that LISA can probe"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"For signal-to-noise ratios ≲100, LISA can distinguish gravitational waveforms from binaries embedded in such halo overdensities; LISA can probe boson masses m_dm∼10^{-17}-10^{-15} eV and decay constants f_a∼10^{10}-3.2×10^{12} GeV using binaries with total masses M∼10^4-10^5 M_⊙, assuming conservative DM densities consistent with the central values of Navarro-Frenk-White profiles. For a binary with M∼10^4 M_⊙, ρ_dm=10^3 GeV/cm^3, and SNR∼20, m_dm∼2.5×10^{-16} eV and f_a∼6.3×10^{10} GeV maximize dephasing, enabling percent-level recovery.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The recently proposed dynamical formation mechanism produces gravitational atom halos with background densities at least as high as the central values of Navarro-Frenk-White profiles; if actual densities are substantially lower or the formation mechanism does not apply as assumed, the dynamical friction dephasing falls below detectable levels for the quoted SNR range.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"LISA can distinguish waveforms from extreme-mass-ratio inspirals affected by dynamical friction in axion-like gravitational atom halos, probing boson masses 10^{-17} to 10^{-15} eV and decay constants 10^{10} to 3.2e12 GeV for total masses 10^4-10^5 solar masses under NFW-consistent densities.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Axion-like particles forming halos around black holes cause detectable dephasing in LISA waveforms from inspiraling binaries.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"35980668f61c0fc3932e9126e251b0476d4c34090aa528187fe7406e9232357d"},"source":{"id":"2605.17589","kind":"arxiv","version":1},"verdict":{"id":"bb4e723b-22ea-470f-9e10-4fe19867ec3e","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T22:58:14.352461Z","strongest_claim":"For signal-to-noise ratios ≲100, LISA can distinguish gravitational waveforms from binaries embedded in such halo overdensities; LISA can probe boson masses m_dm∼10^{-17}-10^{-15} eV and decay constants f_a∼10^{10}-3.2×10^{12} GeV using binaries with total masses M∼10^4-10^5 M_⊙, assuming conservative DM densities consistent with the central values of Navarro-Frenk-White profiles. For a binary with M∼10^4 M_⊙, ρ_dm=10^3 GeV/cm^3, and SNR∼20, m_dm∼2.5×10^{-16} eV and f_a∼6.3×10^{10} GeV maximize dephasing, enabling percent-level recovery.","one_line_summary":"LISA can distinguish waveforms from extreme-mass-ratio inspirals affected by dynamical friction in axion-like gravitational atom halos, probing boson masses 10^{-17} to 10^{-15} eV and decay constants 10^{10} to 3.2e12 GeV for total masses 10^4-10^5 solar masses under NFW-consistent densities.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The recently proposed dynamical formation mechanism produces gravitational atom halos with background densities at least as high as the central values of Navarro-Frenk-White profiles; if actual densities are substantially lower or the formation mechanism does not apply as assumed, the dynamical friction dephasing falls below detectable levels for the quoted SNR range.","pith_extraction_headline":"Axion-like particles forming halos around black holes cause detectable dephasing in LISA waveforms from inspiraling binaries."},"integrity":{"clean":false,"summary":{"advisory":1,"critical":0,"by_detector":{"doi_compliance":{"total":1,"advisory":1,"critical":0,"informational":0}},"informational":0},"endpoint":"/pith/2605.17589/integrity.json","findings":[{"note":"DOI in the printed bibliography is fragmented by whitespace or line breaks. A longer candidate (10.1103/phys-revd.76.084001) was visible in the surrounding text but could not be confirmed against doi.org as printed.","detector":"doi_compliance","severity":"advisory","ref_index":42,"audited_at":"2026-05-19T23:11:26.348966Z","detected_doi":"10.1103/phys-revd.76.084001","finding_type":"recoverable_identifier","verdict_class":"incontrovertible","detected_arxiv_id":null}],"available":true,"detectors_run":[{"name":"doi_title_agreement","ran_at":"2026-05-19T23:31:19.845722Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_compliance","ran_at":"2026-05-19T23:11:26.348966Z","status":"completed","version":"1.0.0","findings_count":1},{"name":"ai_meta_artifact","ran_at":"2026-05-19T21:33:23.584474Z","status":"skipped","version":"1.0.0","findings_count":0},{"name":"claim_evidence","ran_at":"2026-05-19T21:21:57.513743Z","status":"completed","version":"1.0.0","findings_count":0}],"snapshot_sha256":"c57bd0bbc54c84849236e836b58a628725e2cf2d8f39ed6988176519d3f7eae9"},"references":{"count":57,"sample":[{"doi":"","year":null,"title":"These were calculated by recovering different param- eter injections in logL. By marking in gray the region where we have computed the mismatchM(h BG|hGA), whereh v is the strain in vacuum andh GA is ","work_id":"c386e41f-76ff-40d9-99f8-ed1cbc84b3c1","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.13039/501100011033","year":2024,"title":"Using a Fisher Matrix framework, we have studied the frac- tional uncertaintiesσ θi /θi change for bothm dm","work_id":"dd544aa1-fa7d-44a2-9d86-6421740a1e1e","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1140/epjc/s10052-024-13672-y","year":2025,"title":"G. Arcadi, D. Cabo-Almeida, M. Dutra, P. Ghosh, M. Lindner, Y. Mambrini, J. P. Neto, M. Pierre, S. Pro- fumo, and F. S. Queiroz, The European Physical Journal C85(2025), 10.1140/epjc/s10052-024-13672-","work_id":"f471786d-a571-45e8-93e2-e0139de4fb5f","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"10.1007/s00159-021-00135-6","year":2021,"title":"E. G. M. 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