{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:OSR2YIW3UQNIGVML5YO3HXIXBJ","short_pith_number":"pith:OSR2YIW3","schema_version":"1.0","canonical_sha256":"74a3ac22dba41a83558bee1db3dd170a75e1a3face4d9ae6463b8113435905d9","source":{"kind":"arxiv","id":"1906.11848","version":2},"attestation_state":"computed","paper":{"title":"Ultra-light Dark Matter is Incompatible with the Milky Way's Dwarf Satellites","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"David N. Spergel, Mohammadtaher Safarzadeh","submitted_at":"2019-06-27T18:00:05Z","abstract_excerpt":"The density profiles of dwarf galaxies are a highly varied set. If the dark matter is an ultra-light particle such as axions, then simulations predict a distinctive and unique profile. If the axion mass is large enough to fit the ultra-faint dwarf (UFD) satellites($m\\gtrapprox 10^{-21}$ eV), then the models do not fit the density profile of Fornax and Sculptor and are ruled out by more than $3-\\sigma$ confidence. If the axion mass is in the mass range that can fit mass profiles of Fornax and Sculptor dwarf spheroidals, then its extended profile implies enormous masses ($\\approx10^{11}-10^{12}M"},"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":"1906.11848","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-06-27T18:00:05Z","cross_cats_sorted":["astro-ph.GA","hep-ph"],"title_canon_sha256":"acb725ff6d62974be4bf008933d589249cd0719b05061ddc75151c215dff1a27","abstract_canon_sha256":"bf3a4cf9b79fc3fc96ace909fd6aa6a4acb3c0b19a3b6feb47f3497c335b85d8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:55:02.516686Z","signature_b64":"afR/ubI8P1IQjVW4qn2IoMz80wQa3Lcm71+itY7TZolPyaWqZJnOxN5QW6BGLZjNui/250ScPsVT7/RuMC2iCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"74a3ac22dba41a83558bee1db3dd170a75e1a3face4d9ae6463b8113435905d9","last_reissued_at":"2026-07-05T00:55:02.516166Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:55:02.516166Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Ultra-light Dark Matter is Incompatible with the Milky Way's Dwarf Satellites","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"David N. Spergel, Mohammadtaher Safarzadeh","submitted_at":"2019-06-27T18:00:05Z","abstract_excerpt":"The density profiles of dwarf galaxies are a highly varied set. If the dark matter is an ultra-light particle such as axions, then simulations predict a distinctive and unique profile. If the axion mass is large enough to fit the ultra-faint dwarf (UFD) satellites($m\\gtrapprox 10^{-21}$ eV), then the models do not fit the density profile of Fornax and Sculptor and are ruled out by more than $3-\\sigma$ confidence. If the axion mass is in the mass range that can fit mass profiles of Fornax and Sculptor dwarf spheroidals, then its extended profile implies enormous masses ($\\approx10^{11}-10^{12}M"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1906.11848","kind":"arxiv","version":2},"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/1906.11848/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":"1906.11848","created_at":"2026-07-05T00:55:02.516243+00:00"},{"alias_kind":"arxiv_version","alias_value":"1906.11848v2","created_at":"2026-07-05T00:55:02.516243+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1906.11848","created_at":"2026-07-05T00:55:02.516243+00:00"},{"alias_kind":"pith_short_12","alias_value":"OSR2YIW3UQNI","created_at":"2026-07-05T00:55:02.516243+00:00"},{"alias_kind":"pith_short_16","alias_value":"OSR2YIW3UQNIGVML","created_at":"2026-07-05T00:55:02.516243+00:00"},{"alias_kind":"pith_short_8","alias_value":"OSR2YIW3","created_at":"2026-07-05T00:55:02.516243+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.12589","citing_title":"Tunneling and tidal stripping in multifield ultralight dark matter halos","ref_index":34,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26393","citing_title":"Tidal Heating of Stellar Clusters in Fuzzy Dark Matter Halos","ref_index":32,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ","json":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ.json","graph_json":"https://pith.science/api/pith-number/OSR2YIW3UQNIGVML5YO3HXIXBJ/graph.json","events_json":"https://pith.science/api/pith-number/OSR2YIW3UQNIGVML5YO3HXIXBJ/events.json","paper":"https://pith.science/paper/OSR2YIW3"},"agent_actions":{"view_html":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ","download_json":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ.json","view_paper":"https://pith.science/paper/OSR2YIW3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1906.11848&json=true","fetch_graph":"https://pith.science/api/pith-number/OSR2YIW3UQNIGVML5YO3HXIXBJ/graph.json","fetch_events":"https://pith.science/api/pith-number/OSR2YIW3UQNIGVML5YO3HXIXBJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ/action/storage_attestation","attest_author":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ/action/author_attestation","sign_citation":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ/action/citation_signature","submit_replication":"https://pith.science/pith/OSR2YIW3UQNIGVML5YO3HXIXBJ/action/replication_record"}},"created_at":"2026-07-05T00:55:02.516243+00:00","updated_at":"2026-07-05T00:55:02.516243+00:00"}