{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:CEYLU3TWFB6F2ZJZGQRI3RBCG7","short_pith_number":"pith:CEYLU3TW","schema_version":"1.0","canonical_sha256":"1130ba6e76287c5d653934228dc42237f09126845d533c7311c15da1596267c0","source":{"kind":"arxiv","id":"2605.15371","version":1},"attestation_state":"computed","paper":{"title":"Warm, not Fuzzy: Generalized Ultralight Dark Matter Limits from Milky Way Satellites","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Milky Way satellite abundances set mass limits on ultralight dark matter that scale with the initial power spectrum peak wavenumber.","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Andrew Benson, Ethan O. Nadler, M. Sten Delos, Mustafa A. Amin, Risa H. Wechsler, Vera Gluscevic","submitted_at":"2026-05-14T19:53:04Z","abstract_excerpt":"We generalize lower limits on the dark matter (DM) particle mass $m$ derived from Milky Way (MW) satellite galaxy abundances to scenarios in which DM is an ultralight scalar field produced with a field power spectrum peaked at a subhorizon wavenumber $k_*$. In these models, the DM field free-streams similar to warm dark matter while also exhibiting significant small-scale wave interference effects. The resulting dimensionless density power spectrum shows two effects: (i) free-streaming suppression at $k_{\\rm fs}\\sim k_{\\rm eq}/[(k_*/a_{\\rm eq}m)\\ln(a_{\\rm eq}m/k_*)]$; (ii) Poisson-like enhance"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":true,"formal_links_present":true},"canonical_record":{"source":{"id":"2605.15371","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T19:53:04Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"cc5ab50ad82a58fb43d5870502344476b5ef9669b4bdcf09b746b16d4e8f9b76","abstract_canon_sha256":"a502b0684c3009a37b2b106b7c344ca203cf2076ba4de726b0ec2e5a99f85dc8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-20T00:00:55.047001Z","signature_b64":"uWQJ21pT8o87F2kcnWgW4h+m7mHdLbePwDKXAmQGcJfLQlG7+LHn3YNs7dAL+vkjMpNXUE4kqNGlSQUEEwtPBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"1130ba6e76287c5d653934228dc42237f09126845d533c7311c15da1596267c0","last_reissued_at":"2026-05-20T00:00:55.046098Z","signature_status":"signed_v1","first_computed_at":"2026-05-20T00:00:55.046098Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Warm, not Fuzzy: Generalized Ultralight Dark Matter Limits from Milky Way Satellites","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Milky Way satellite abundances set mass limits on ultralight dark matter that scale with the initial power spectrum peak wavenumber.","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Andrew Benson, Ethan O. Nadler, M. Sten Delos, Mustafa A. Amin, Risa H. Wechsler, Vera Gluscevic","submitted_at":"2026-05-14T19:53:04Z","abstract_excerpt":"We generalize lower limits on the dark matter (DM) particle mass $m$ derived from Milky Way (MW) satellite galaxy abundances to scenarios in which DM is an ultralight scalar field produced with a field power spectrum peaked at a subhorizon wavenumber $k_*$. In these models, the DM field free-streams similar to warm dark matter while also exhibiting significant small-scale wave interference effects. The resulting dimensionless density power spectrum shows two effects: (i) free-streaming suppression at $k_{\\rm fs}\\sim k_{\\rm eq}/[(k_*/a_{\\rm eq}m)\\ln(a_{\\rm eq}m/k_*)]$; (ii) Poisson-like enhance"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"Comparing these predictions with established constraints on a free-streaming cutoff in the linear matter power spectrum from the MW satellite population, we obtain m>6×10^{-18} eV (k_*/10^4 Mpc^{-1}) for k_*>10^4 Mpc^{-1} at 95% confidence. For smaller k_*, ... m>6×10^{-18} eV (k_*/10^4 Mpc^{-1})^2.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"That the free-streaming suppression scale k_fs and the Poisson enhancement from wave interference can be directly translated into an effective free-streaming cutoff that matches the functional form assumed in prior MW satellite abundance analyses without requiring new modeling of satellite formation or selection in the generalized power spectrum.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Generalizes ultralight DM mass limits from MW satellite abundances to peaked power spectrum models, yielding m > 6e-18 eV scaled by k_* at 95% confidence for different k_* regimes.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Milky Way satellite abundances set mass limits on ultralight dark matter that scale with the initial power spectrum peak wavenumber.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"a3017b70785d7f4f74fb02e1895f050441aaff6f1a1d27f4219f7724b3d81129"},"source":{"id":"2605.15371","kind":"arxiv","version":1},"verdict":{"id":"f591afe8-6633-4710-a8ae-36650fde1ffb","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-19T15:24:53.332758Z","strongest_claim":"Comparing these predictions with established constraints on a free-streaming cutoff in the linear matter power spectrum from the MW satellite population, we obtain m>6×10^{-18} eV (k_*/10^4 Mpc^{-1}) for k_*>10^4 Mpc^{-1} at 95% confidence. For smaller k_*, ... m>6×10^{-18} eV (k_*/10^4 Mpc^{-1})^2.","one_line_summary":"Generalizes ultralight DM mass limits from MW satellite abundances to peaked power spectrum models, yielding m > 6e-18 eV scaled by k_* at 95% confidence for different k_* regimes.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"That the free-streaming suppression scale k_fs and the Poisson enhancement from wave interference can be directly translated into an effective free-streaming cutoff that matches the functional form assumed in prior MW satellite abundance analyses without requiring new modeling of satellite formation or selection in the generalized power spectrum.","pith_extraction_headline":"Milky Way satellite abundances set mass limits on ultralight dark matter that scale with the initial power spectrum peak wavenumber."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2605.15371/integrity.json","findings":[],"available":true,"detectors_run":[{"name":"doi_title_agreement","ran_at":"2026-05-19T15:31:17.879935Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"doi_compliance","ran_at":"2026-05-19T15:30:47.495119Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"claim_evidence","ran_at":"2026-05-19T14:21:54.186589Z","status":"completed","version":"1.0.0","findings_count":0},{"name":"ai_meta_artifact","ran_at":"2026-05-19T13:33:22.735800Z","status":"skipped","version":"1.0.0","findings_count":0}],"snapshot_sha256":"0e7a276c2597e879973d6f87570495ced3cff1cf7f12d13050edd8cf85533554"},"references":{"count":39,"sample":[{"doi":"","year":2014,"title":"2014, JCAP, 10, 002","work_id":"d8a61412-94bc-49e0-9d30-acc2fcd140d5","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2025,"title":"Amin, M. A. & Delos, M. S. 2025, arXiv e-prints, arXiv:2510.17977","work_id":"839b86c0-f3a1-4cce-adad-45398cecd5c2","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2026,"title":"Amin, M. A., Delos, M. S., & Mirbabayi, M. 2026, JCAP, 2026, 016","work_id":"a46dc0be-6149-4697-9f5a-c6a88c013881","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"Amin, M. A., Delos, M. S., & Yang, K. 2025a, arXiv e-prints, arXiv:2510.15046","work_id":"e56aa73a-482f-49b0-bb11-696757eaa458","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2025,"title":"A., May, S., & Mirbabayi, M","work_id":"f9c7d9b9-e2ed-4369-93cc-06fcd5ad87f6","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":39,"snapshot_sha256":"08a8362bb1be718633f06f19ecfdd98a43e06fed793973b11cea8ecabf88b02b","internal_anchors":0},"formal_canon":{"evidence_count":2,"snapshot_sha256":"f13b276ca8a9abf2b965195e8d6a2f6a61f3726c8a22643aa0b78fd084a02b40"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2605.15371","created_at":"2026-05-20T00:00:55.046259+00:00"},{"alias_kind":"arxiv_version","alias_value":"2605.15371v1","created_at":"2026-05-20T00:00:55.046259+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2605.15371","created_at":"2026-05-20T00:00:55.046259+00:00"},{"alias_kind":"pith_short_12","alias_value":"CEYLU3TWFB6F","created_at":"2026-05-20T00:00:55.046259+00:00"},{"alias_kind":"pith_short_16","alias_value":"CEYLU3TWFB6F2ZJZ","created_at":"2026-05-20T00:00:55.046259+00:00"},{"alias_kind":"pith_short_8","alias_value":"CEYLU3TW","created_at":"2026-05-20T00:00:55.046259+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":2,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7","json":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7.json","graph_json":"https://pith.science/api/pith-number/CEYLU3TWFB6F2ZJZGQRI3RBCG7/graph.json","events_json":"https://pith.science/api/pith-number/CEYLU3TWFB6F2ZJZGQRI3RBCG7/events.json","paper":"https://pith.science/paper/CEYLU3TW"},"agent_actions":{"view_html":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7","download_json":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7.json","view_paper":"https://pith.science/paper/CEYLU3TW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2605.15371&json=true","fetch_graph":"https://pith.science/api/pith-number/CEYLU3TWFB6F2ZJZGQRI3RBCG7/graph.json","fetch_events":"https://pith.science/api/pith-number/CEYLU3TWFB6F2ZJZGQRI3RBCG7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7/action/storage_attestation","attest_author":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7/action/author_attestation","sign_citation":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7/action/citation_signature","submit_replication":"https://pith.science/pith/CEYLU3TWFB6F2ZJZGQRI3RBCG7/action/replication_record"}},"created_at":"2026-05-20T00:00:55.046259+00:00","updated_at":"2026-05-20T00:00:55.046259+00:00"}