{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:X5YODYCVZQ3YCCQ5IWNPZZ7MRI","short_pith_number":"pith:X5YODYCV","schema_version":"1.0","canonical_sha256":"bf70e1e055cc37810a1d459afce7ec8a1be15e06525d789c540ebdf39fedd3d3","source":{"kind":"arxiv","id":"1301.1864","version":3},"attestation_state":"computed","paper":{"title":"Quantum WDM fermions and gravitation determine the observed galaxy structures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"C. Destri, H. J. de Vega, N. G. Sanchez","submitted_at":"2013-01-07T21:00:01Z","abstract_excerpt":"Quantum mechanics is necessary to compute galaxy structures at kpc scales and below. This is so because near the galaxy center, at scales below 10 - 100 pc, warm dark matter (WDM) quantum effects are important: observations show that the interparticle distance is of the order of, or smaller than the de Broglie wavelength for WDM. This explains why all classical (non-quantum) WDM N-body simulations fail to explain galactic cores and their sizes. We describe fermionic WDM galaxies in an analytic semiclassical framework based on the Thomas-Fermi approach, we resolve it numerically and find the ma"},"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":"1301.1864","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-01-07T21:00:01Z","cross_cats_sorted":["gr-qc","hep-ph"],"title_canon_sha256":"f3898abb83d1e6b100a890c7875d3a0ce7e6ff0ca0d0b0b7ea56055fb082c5af","abstract_canon_sha256":"f1d6a0298ae2b1328a0d18b9fd6632b4cc17f850eed640b7e8f336910f2acc0a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:52:14.429056Z","signature_b64":"gG4UZg1mfcdUgdewp6de86JO+NvbkOAXLFTEpHrS1lO9duhRAL1M0cL8kpQz0i83N8fDe5V0IMaTiFUnnfflDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bf70e1e055cc37810a1d459afce7ec8a1be15e06525d789c540ebdf39fedd3d3","last_reissued_at":"2026-05-18T01:52:14.428299Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:52:14.428299Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Quantum WDM fermions and gravitation determine the observed galaxy structures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"C. Destri, H. J. de Vega, N. G. Sanchez","submitted_at":"2013-01-07T21:00:01Z","abstract_excerpt":"Quantum mechanics is necessary to compute galaxy structures at kpc scales and below. This is so because near the galaxy center, at scales below 10 - 100 pc, warm dark matter (WDM) quantum effects are important: observations show that the interparticle distance is of the order of, or smaller than the de Broglie wavelength for WDM. This explains why all classical (non-quantum) WDM N-body simulations fail to explain galactic cores and their sizes. We describe fermionic WDM galaxies in an analytic semiclassical framework based on the Thomas-Fermi approach, we resolve it numerically and find the ma"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1301.1864","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"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":"1301.1864","created_at":"2026-05-18T01:52:14.428434+00:00"},{"alias_kind":"arxiv_version","alias_value":"1301.1864v3","created_at":"2026-05-18T01:52:14.428434+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1301.1864","created_at":"2026-05-18T01:52:14.428434+00:00"},{"alias_kind":"pith_short_12","alias_value":"X5YODYCVZQ3Y","created_at":"2026-05-18T12:28:06.772260+00:00"},{"alias_kind":"pith_short_16","alias_value":"X5YODYCVZQ3YCCQ5","created_at":"2026-05-18T12:28:06.772260+00:00"},{"alias_kind":"pith_short_8","alias_value":"X5YODYCV","created_at":"2026-05-18T12:28:06.772260+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"1906.10316","citing_title":"Constraining light fermionic dark matter with binary pulsars","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2407.01690","citing_title":"Structure-wide dark matter density depletion induced by local degeneracies","ref_index":21,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI","json":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI.json","graph_json":"https://pith.science/api/pith-number/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/graph.json","events_json":"https://pith.science/api/pith-number/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/events.json","paper":"https://pith.science/paper/X5YODYCV"},"agent_actions":{"view_html":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI","download_json":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI.json","view_paper":"https://pith.science/paper/X5YODYCV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1301.1864&json=true","fetch_graph":"https://pith.science/api/pith-number/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/graph.json","fetch_events":"https://pith.science/api/pith-number/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/action/storage_attestation","attest_author":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/action/author_attestation","sign_citation":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/action/citation_signature","submit_replication":"https://pith.science/pith/X5YODYCVZQ3YCCQ5IWNPZZ7MRI/action/replication_record"}},"created_at":"2026-05-18T01:52:14.428434+00:00","updated_at":"2026-05-18T01:52:14.428434+00:00"}