{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:XVORZ325ZD3BESAMPB3OLIR7OA","short_pith_number":"pith:XVORZ325","schema_version":"1.0","canonical_sha256":"bd5d1cef5dc8f612480c7876e5a23f70355c94852c0e24b9336ab884ffe68401","source":{"kind":"arxiv","id":"astro-ph/0308385","version":2},"attestation_state":"computed","paper":{"title":"Dark Matter Profile in the Galactic Center","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Joel R. Primack (UC Santa Cruz), Oleg Y. Gnedin (STScI)","submitted_at":"2003-08-21T20:01:02Z","abstract_excerpt":"We describe a quasi-equilibrium profile of dark matter particles in the inner parsec of the Galaxy, rho ~ r^-3/2. This \"mini-cusp\" profile is caused by scattering with the dense stellar cluster around the supermassive black hole in Sgr A* and is independent of the initial conditions. The implications for detection of gamma rays from WIMP dark matter annihilation in the Galactic center are a mild enhancement of the flux, and a characteristic central feature in the angular distribution which could be detectable by high-resolution Atmospheric Cherenkov Telescopes."},"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":"astro-ph/0308385","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-08-21T20:01:02Z","cross_cats_sorted":[],"title_canon_sha256":"379592977f8609f64220bd9ea511d2120b5a8c7da9ff83e89f5d0334bf914f63","abstract_canon_sha256":"ae9763766fb1af9926203d41d47d5542a192a77eb092a35b168943c39ce62056"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:51:30.440388Z","signature_b64":"jiPSLTm2Qp3ywbhSqC3hwrGQ1NKT4xPYZ4xw6acCwRMzsOqetlZpHaGI6VKltnFCJNeDKnEj9AB65v1h1Hw0Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bd5d1cef5dc8f612480c7876e5a23f70355c94852c0e24b9336ab884ffe68401","last_reissued_at":"2026-07-04T16:51:30.439971Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:51:30.439971Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dark Matter Profile in the Galactic Center","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Joel R. Primack (UC Santa Cruz), Oleg Y. Gnedin (STScI)","submitted_at":"2003-08-21T20:01:02Z","abstract_excerpt":"We describe a quasi-equilibrium profile of dark matter particles in the inner parsec of the Galaxy, rho ~ r^-3/2. This \"mini-cusp\" profile is caused by scattering with the dense stellar cluster around the supermassive black hole in Sgr A* and is independent of the initial conditions. The implications for detection of gamma rays from WIMP dark matter annihilation in the Galactic center are a mild enhancement of the flux, and a characteristic central feature in the angular distribution which could be detectable by high-resolution Atmospheric Cherenkov Telescopes."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0308385","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/astro-ph/0308385/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":"astro-ph/0308385","created_at":"2026-07-04T16:51:30.440025+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0308385v2","created_at":"2026-07-04T16:51:30.440025+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0308385","created_at":"2026-07-04T16:51:30.440025+00:00"},{"alias_kind":"pith_short_12","alias_value":"XVORZ325ZD3B","created_at":"2026-07-04T16:51:30.440025+00:00"},{"alias_kind":"pith_short_16","alias_value":"XVORZ325ZD3BESAM","created_at":"2026-07-04T16:51:30.440025+00:00"},{"alias_kind":"pith_short_8","alias_value":"XVORZ325","created_at":"2026-07-04T16:51:30.440025+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2607.00840","citing_title":"Dark matter energy exchange in stars orbiting supermassive black holes","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2509.03568","citing_title":"Probing dense environments around Sgr A* with S-stars dynamics","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2510.27424","citing_title":"Extracting Properties of Dark Dense Environments around Black Holes from Gravitational Waves","ref_index":50,"is_internal_anchor":true},{"citing_arxiv_id":"2511.07567","citing_title":"Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach","ref_index":16,"is_internal_anchor":true},{"citing_arxiv_id":"2604.25961","citing_title":"Strong-field signatures of a regular black hole in an Einasto dark matter halo","ref_index":23,"is_internal_anchor":false},{"citing_arxiv_id":"2605.01023","citing_title":"Formation and Redshift Evolution of Dark Matter Spikes","ref_index":74,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA","json":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA.json","graph_json":"https://pith.science/api/pith-number/XVORZ325ZD3BESAMPB3OLIR7OA/graph.json","events_json":"https://pith.science/api/pith-number/XVORZ325ZD3BESAMPB3OLIR7OA/events.json","paper":"https://pith.science/paper/XVORZ325"},"agent_actions":{"view_html":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA","download_json":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA.json","view_paper":"https://pith.science/paper/XVORZ325","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0308385&json=true","fetch_graph":"https://pith.science/api/pith-number/XVORZ325ZD3BESAMPB3OLIR7OA/graph.json","fetch_events":"https://pith.science/api/pith-number/XVORZ325ZD3BESAMPB3OLIR7OA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA/action/storage_attestation","attest_author":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA/action/author_attestation","sign_citation":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA/action/citation_signature","submit_replication":"https://pith.science/pith/XVORZ325ZD3BESAMPB3OLIR7OA/action/replication_record"}},"created_at":"2026-07-04T16:51:30.440025+00:00","updated_at":"2026-07-04T16:51:30.440025+00:00"}