{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:SZM5UV3SPGWJY5NLS5SHCTLMXB","short_pith_number":"pith:SZM5UV3S","schema_version":"1.0","canonical_sha256":"9659da577279ac9c75ab9764714d6cb87f17e54d3a6daac786b3164c06358c7f","source":{"kind":"arxiv","id":"2509.02781","version":1},"attestation_state":"computed","paper":{"title":"Updated bounds on ultra-light dark matter from the tiniest galaxies","license":"http://creativecommons.org/licenses/by-sa/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Andrey Kravtsov, Neal Dalal, Simon May","submitted_at":"2025-09-02T19:35:25Z","abstract_excerpt":"The particle mass of dark matter (DM) was previously constrained using kinematics of ultra-faint dwarf galaxies to $m > 3 \\times 10^{-19}\\,\\mathrm{eV}$. This constraint, which excludes the \"fuzzy\" range of ultra-light dark matter from comprising all of the DM, relies on an estimate of the heating rate from fuzzy dark matter (FDM) wave interference using linear perturbation theory. Here, we compare the results of this perturbative calculation to full Schr\\\"odinger-Poisson simulations of the evolution of star particles in FDM halos. This comparison confirms theoretical expectations that FDM heat"},"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":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2509.02781","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-sa/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-09-02T19:35:25Z","cross_cats_sorted":["astro-ph.GA","hep-ph"],"title_canon_sha256":"15a9adf23c846f937cfec899f00d40cc74be353904dd8eacbd627c679fc47494","abstract_canon_sha256":"54319343eedb259bb091ae898a2d65aeeb5a6c058ae27f047e928c35d7d49d45"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T12:05:22.090574Z","signature_b64":"lJDNqxVfff7S4HPkwV+8nS2nSBPZcasqKNrP0wscq7ZIUcQmtTG97lVMylFwFIx6RszewAzLirMYUFEjYIggAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9659da577279ac9c75ab9764714d6cb87f17e54d3a6daac786b3164c06358c7f","last_reissued_at":"2026-07-05T12:05:22.090083Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T12:05:22.090083Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Updated bounds on ultra-light dark matter from the tiniest galaxies","license":"http://creativecommons.org/licenses/by-sa/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Andrey Kravtsov, Neal Dalal, Simon May","submitted_at":"2025-09-02T19:35:25Z","abstract_excerpt":"The particle mass of dark matter (DM) was previously constrained using kinematics of ultra-faint dwarf galaxies to $m > 3 \\times 10^{-19}\\,\\mathrm{eV}$. This constraint, which excludes the \"fuzzy\" range of ultra-light dark matter from comprising all of the DM, relies on an estimate of the heating rate from fuzzy dark matter (FDM) wave interference using linear perturbation theory. Here, we compare the results of this perturbative calculation to full Schr\\\"odinger-Poisson simulations of the evolution of star particles in FDM halos. This comparison confirms theoretical expectations that FDM heat"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2509.02781","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2509.02781/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"2509.02781","created_at":"2026-07-05T12:05:22.090139+00:00"},{"alias_kind":"arxiv_version","alias_value":"2509.02781v1","created_at":"2026-07-05T12:05:22.090139+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2509.02781","created_at":"2026-07-05T12:05:22.090139+00:00"},{"alias_kind":"pith_short_12","alias_value":"SZM5UV3SPGWJ","created_at":"2026-07-05T12:05:22.090139+00:00"},{"alias_kind":"pith_short_16","alias_value":"SZM5UV3SPGWJY5NL","created_at":"2026-07-05T12:05:22.090139+00:00"},{"alias_kind":"pith_short_8","alias_value":"SZM5UV3S","created_at":"2026-07-05T12:05:22.090139+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":8,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.06410","citing_title":"The Atacama Cosmology Telescope: Probing new signatures of ultralight axions with gravitational lensing","ref_index":43,"is_internal_anchor":false},{"citing_arxiv_id":"2606.29149","citing_title":"Evolution of Compact Stellar Systems in Ultralight Dark Matter Halos: Dependence on Stellar and Dark Matter Parameters","ref_index":27,"is_internal_anchor":false},{"citing_arxiv_id":"2606.06599","citing_title":"Halo mass functions in mixed cold and fuzzy dark matter models","ref_index":61,"is_internal_anchor":false},{"citing_arxiv_id":"2510.17977","citing_title":"Growth of Structure in Multi-species Wave Dark Matter","ref_index":83,"is_internal_anchor":false},{"citing_arxiv_id":"2605.17211","citing_title":"Constraints on Self-Interacting Fuzzy Dark Matter from the Stellar Kinematics of the Dwarf Galaxy Leo II","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2602.11512","citing_title":"Stone Skipping Black Holes in Ultralight Dark Matter Solitons","ref_index":37,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26393","citing_title":"Tidal Heating of Stellar Clusters in Fuzzy Dark Matter Halos","ref_index":25,"is_internal_anchor":false},{"citing_arxiv_id":"2605.06777","citing_title":"Neutrino-Antineutrino Conversion from Ultralight Vector Dark Matter","ref_index":97,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB","json":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB.json","graph_json":"https://pith.science/api/pith-number/SZM5UV3SPGWJY5NLS5SHCTLMXB/graph.json","events_json":"https://pith.science/api/pith-number/SZM5UV3SPGWJY5NLS5SHCTLMXB/events.json","paper":"https://pith.science/paper/SZM5UV3S"},"agent_actions":{"view_html":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB","download_json":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB.json","view_paper":"https://pith.science/paper/SZM5UV3S","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2509.02781&json=true","fetch_graph":"https://pith.science/api/pith-number/SZM5UV3SPGWJY5NLS5SHCTLMXB/graph.json","fetch_events":"https://pith.science/api/pith-number/SZM5UV3SPGWJY5NLS5SHCTLMXB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB/action/storage_attestation","attest_author":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB/action/author_attestation","sign_citation":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB/action/citation_signature","submit_replication":"https://pith.science/pith/SZM5UV3SPGWJY5NLS5SHCTLMXB/action/replication_record"}},"created_at":"2026-07-05T12:05:22.090139+00:00","updated_at":"2026-07-05T12:05:22.090139+00:00"}