{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:YAT2O4NNQBKH36ZXFDJ6PJRUCO","short_pith_number":"pith:YAT2O4NN","schema_version":"1.0","canonical_sha256":"c027a771ad80547dfb3728d3e7a6341398d26a3c6e909a36beb9adb076c8db5e","source":{"kind":"arxiv","id":"1204.3622","version":3},"attestation_state":"computed","paper":{"title":"Precise Relic WIMP Abundance and its Impact on Searches for Dark Matter Annihilation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.GA"],"primary_cat":"hep-ph","authors_text":"Basudeb Dasgupta, Gary Steigman, John F. Beacom","submitted_at":"2012-04-16T20:00:00Z","abstract_excerpt":"If dark matter (DM) is a weakly interacting massive particle (WIMP) that is a thermal relic of the early Universe, then its total self-annihilation cross section is revealed by its present-day mass density. The canonical thermally averaged cross section for a generic WIMP is usually stated as 3*10^-26 cm^3s^-1, with unspecified uncertainty, and taken to be independent of WIMP mass. Recent searches for annihilation products of DM annihilation have just reached the sensitivity to exclude this canonical cross section for 100% branching ratio to certain final states and small WIMP masses. The ulti"},"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":"1204.3622","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2012-04-16T20:00:00Z","cross_cats_sorted":["astro-ph.CO","astro-ph.GA"],"title_canon_sha256":"9a5220b777497b91bbcc18cced5c38a818863710ec35f39afa81bb0d4ec0936e","abstract_canon_sha256":"7c002f820b7704a620cdd0936521fb04fd07f25a9b5624852840a2e311cc682d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:49:00.874718Z","signature_b64":"+z7nG4N+Q7RjnmedUfl3uqMjpneT+NKIRYXdj2t5leG6QoEja3b+KJfFYz/Ri+1nAj2ZkBxkA8TjHXifMnTACg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c027a771ad80547dfb3728d3e7a6341398d26a3c6e909a36beb9adb076c8db5e","last_reissued_at":"2026-05-18T03:49:00.874070Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:49:00.874070Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Precise Relic WIMP Abundance and its Impact on Searches for Dark Matter Annihilation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.GA"],"primary_cat":"hep-ph","authors_text":"Basudeb Dasgupta, Gary Steigman, John F. Beacom","submitted_at":"2012-04-16T20:00:00Z","abstract_excerpt":"If dark matter (DM) is a weakly interacting massive particle (WIMP) that is a thermal relic of the early Universe, then its total self-annihilation cross section is revealed by its present-day mass density. The canonical thermally averaged cross section for a generic WIMP is usually stated as 3*10^-26 cm^3s^-1, with unspecified uncertainty, and taken to be independent of WIMP mass. Recent searches for annihilation products of DM annihilation have just reached the sensitivity to exclude this canonical cross section for 100% branching ratio to certain final states and small WIMP masses. The ulti"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1204.3622","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":"1204.3622","created_at":"2026-05-18T03:49:00.874164+00:00"},{"alias_kind":"arxiv_version","alias_value":"1204.3622v3","created_at":"2026-05-18T03:49:00.874164+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1204.3622","created_at":"2026-05-18T03:49:00.874164+00:00"},{"alias_kind":"pith_short_12","alias_value":"YAT2O4NNQBKH","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_16","alias_value":"YAT2O4NNQBKH36ZX","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_8","alias_value":"YAT2O4NN","created_at":"2026-05-18T12:27:27.928770+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":10,"internal_anchor_count":7,"sample":[{"citing_arxiv_id":"1906.11896","citing_title":"Unidentified Gamma-ray Sources as Targets for Indirect Dark Matter Detection with the Fermi-Large Area Telescope","ref_index":92,"is_internal_anchor":true},{"citing_arxiv_id":"1907.04324","citing_title":"Dark Matter Energy Deposition and Production from the Table-Top to the Cosmos","ref_index":39,"is_internal_anchor":true},{"citing_arxiv_id":"2509.07070","citing_title":"Reviving WIMP dark matter with temperature-dependent couplings","ref_index":46,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20162","citing_title":"Dark Matter Interpretation of the Super-Kamiokande Antineutrino Excess and Predictions for JUNO","ref_index":39,"is_internal_anchor":true},{"citing_arxiv_id":"2507.11376","citing_title":"GeV-scale thermal dark matter from dark photons: tightly constrained, yet allowed","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2509.08043","citing_title":"Testing Viability of Benchmark Dark Matter Models for the Galactic Center Excess","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2602.20237","citing_title":"Linking Leptogenesis and Asymmetric Dark Matter: A Testable Framework for Neutrino Mass and the Matter-Antimatter Asymmetry","ref_index":41,"is_internal_anchor":true},{"citing_arxiv_id":"2605.04890","citing_title":"Sensitivity of the Cherenkov Telescope Array Observatory to Gamma-Ray Signals in Dwarf Irregular Galaxies","ref_index":1,"is_internal_anchor":false},{"citing_arxiv_id":"2604.07618","citing_title":"Multi Component Dark Matter in a Minimal Model","ref_index":4,"is_internal_anchor":false},{"citing_arxiv_id":"2604.05016","citing_title":"Electroweak Doublet Dark Matter for a Galactic Halo Gamma-Ray Excess","ref_index":2,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO","json":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO.json","graph_json":"https://pith.science/api/pith-number/YAT2O4NNQBKH36ZXFDJ6PJRUCO/graph.json","events_json":"https://pith.science/api/pith-number/YAT2O4NNQBKH36ZXFDJ6PJRUCO/events.json","paper":"https://pith.science/paper/YAT2O4NN"},"agent_actions":{"view_html":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO","download_json":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO.json","view_paper":"https://pith.science/paper/YAT2O4NN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1204.3622&json=true","fetch_graph":"https://pith.science/api/pith-number/YAT2O4NNQBKH36ZXFDJ6PJRUCO/graph.json","fetch_events":"https://pith.science/api/pith-number/YAT2O4NNQBKH36ZXFDJ6PJRUCO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO/action/storage_attestation","attest_author":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO/action/author_attestation","sign_citation":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO/action/citation_signature","submit_replication":"https://pith.science/pith/YAT2O4NNQBKH36ZXFDJ6PJRUCO/action/replication_record"}},"created_at":"2026-05-18T03:49:00.874164+00:00","updated_at":"2026-05-18T03:49:00.874164+00:00"}