{"paper":{"title":"Constraints on Self-Interacting Fuzzy Dark Matter from the Stellar Kinematics of the Dwarf Galaxy Leo II","license":"http://creativecommons.org/licenses/by/4.0/","headline":"Stellar kinematics in Leo II constrain both the mass and self-interaction strength of fuzzy dark matter particles.","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Peng-fei Yin, Xiao-Jun Bi, Yi Zhao, Yu-Ming Yang","submitted_at":"2026-05-17T01:00:54Z","abstract_excerpt":"The one-parameter fuzzy dark matter (FDM) model has faced increasingly stringent constraints from both Lyman-$\\alpha$ forest observations and local measurements of dwarf galaxies. A natural extension to mitigate these limits is the inclusion of FDM self-interactions. In this study, we derive constraints in the two-dimensional parameter space $(m_a, f_a)$ using the dark matter density profile inferred from a Jeans analysis of the stellar kinematics in the dwarf galaxy Leo II, which has previously been employed to constrain non-interacting FDM. We find that, for a fixed particle mass $m_a$, attr"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"For either attractive or repulsive self-interaction with strength f_a^{-1} ≲ 10^{-14} GeV^{-1}, the 95% confidence-level lower limits on m_a lie within the range (1-10)×10^{-22} eV, with the precise bounds depending on the statistical method employed.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The Jeans analysis that supplies the target dark-matter density profile assumes spherical symmetry, dynamical equilibrium, and a specific stellar velocity anisotropy profile; any violation of these assumptions would shift the inferred central density and thereby alter the derived (m_a, f_a) bounds.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Using Jeans analysis of Leo II stellar kinematics, the paper constrains the fuzzy dark matter mass m_a and self-interaction parameter f_a, finding 95% CL lower limits on m_a in the (1-10)×10^{-22} eV range for |f_a^{-1}| ≲ 10^{-14} GeV^{-1}.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Stellar kinematics in Leo II constrain both the mass and self-interaction strength of fuzzy dark matter particles.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"712aa069c74879fe43499878cba3c38a2f1b2a1d075b03959be8b007fa51cea1"},"source":{"id":"2605.17211","kind":"arxiv","version":1},"verdict":{"id":"fab0e079-15ab-433f-946e-a34f9932c782","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T23:31:03.487897Z","strongest_claim":"For either attractive or repulsive self-interaction with strength f_a^{-1} ≲ 10^{-14} GeV^{-1}, the 95% confidence-level lower limits on m_a lie within the range (1-10)×10^{-22} eV, with the precise bounds depending on the statistical method employed.","one_line_summary":"Using Jeans analysis of Leo II stellar kinematics, the paper constrains the fuzzy dark matter mass m_a and self-interaction parameter f_a, finding 95% CL lower limits on m_a in the (1-10)×10^{-22} eV range for |f_a^{-1}| ≲ 10^{-14} GeV^{-1}.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The Jeans analysis that supplies the target dark-matter density profile assumes spherical symmetry, dynamical equilibrium, and a specific stellar velocity anisotropy profile; any violation of these assumptions would shift the inferred central density and thereby alter the derived (m_a, f_a) bounds.","pith_extraction_headline":"Stellar kinematics in Leo II constrain both the mass and self-interaction strength of fuzzy dark matter particles."},"integrity":{"clean":false,"summary":{"advisory":1,"critical":0,"by_detector":{"doi_compliance":{"total":1,"advisory":1,"critical":0,"informational":0}},"informational":0},"endpoint":"/pith/2605.17211/integrity.json","findings":[{"note":"DOI in the printed bibliography is fragmented by whitespace or line breaks. 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Gruzinov, Fuzzy Cold Dark Matter: The Wave Properties of Ultralight Particles, Physical Review Letters85, 1158–1161 (2000)","work_id":"ab91e977-3aba-40f7-b50a-607709305b3e","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2000,"title":"Fluid Dark Matter","work_id":"cc29cefe-0b7e-412e-a5dd-e8830f6c5bdc","ref_index":3,"cited_arxiv_id":"astro-ph/0002495","is_internal_anchor":true},{"doi":"10.1103/physrevd.95.043541","year":2017,"title":"P., Tremaine, S., & Witten, E","work_id":"6a6699bc-7d38-4b0d-86b3-26eade8fd1b2","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2021,"title":"Hui, Wave Dark Matter, Annual Review of Astronomy and Astrophysics59, 247–289 (2021)","work_id":"75e0a75a-9387-4061-ab94-b456964808b2","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":52,"snapshot_sha256":"f39d7cc7e7f77cc4a2b441d3728a7597a1be19e4e0875cb91baa2c1d5db95b8d","internal_anchors":15},"formal_canon":{"evidence_count":2,"snapshot_sha256":"7adcde50cb505668282e2c626b6e4a9fe74d58cb64901c6df50dec195ab3a076"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}