{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1995:HSS2JMAUVEQ35ORHBNBZZSEL6L","short_pith_number":"pith:HSS2JMAU","schema_version":"1.0","canonical_sha256":"3ca5a4b014a921beba270b439cc88bf2d576735d51c1d602bedf5acc5a2c03c5","source":{"kind":"arxiv","id":"astro-ph/9509122","version":2},"attestation_state":"computed","paper":{"title":"Analytical Models For Galactic Nuclei","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"HongSheng Zhao (MPA-Garching)","submitted_at":"1995-09-25T12:26:40Z","abstract_excerpt":"I present a general family of dynamical models with simple analytical potential-density pairs suited to model galactic bulges and nuclei with double power-law radial density profiles and an optional central black hole. Analytical expressions for the potential and velocity dispersion of these models are given in the spherical case. Many previously known analytical spherical models, including also the recent $\\gamma / \\eta$-models by Dehnen (1993) and Tremaine et al. (1994), are special cases of this family. This family also forms a complete set for constructing general galaxy models or solving "},"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/9509122","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1995-09-25T12:26:40Z","cross_cats_sorted":[],"title_canon_sha256":"e023fce98c10c2e883a409f81373d24fda67d561c0771c1b013fdc0705ae96d2","abstract_canon_sha256":"6322368db54a605e36f404a66f2436fe52e855cb076b78fff6abfd0ea3d23d84"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:40:22.673720Z","signature_b64":"160dPyvdPB+M8/TzXPYY1Q1+ElNzsr2HKa7z74Gl2efi/Phsy6L5OMyf0cWvVi9dVeAPypgrzjaBqQ1hZPoACw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3ca5a4b014a921beba270b439cc88bf2d576735d51c1d602bedf5acc5a2c03c5","last_reissued_at":"2026-05-18T01:40:22.672991Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:40:22.672991Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Analytical Models For Galactic Nuclei","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"HongSheng Zhao (MPA-Garching)","submitted_at":"1995-09-25T12:26:40Z","abstract_excerpt":"I present a general family of dynamical models with simple analytical potential-density pairs suited to model galactic bulges and nuclei with double power-law radial density profiles and an optional central black hole. Analytical expressions for the potential and velocity dispersion of these models are given in the spherical case. Many previously known analytical spherical models, including also the recent $\\gamma / \\eta$-models by Dehnen (1993) and Tremaine et al. (1994), are special cases of this family. This family also forms a complete set for constructing general galaxy models or solving "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9509122","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":""},"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/9509122","created_at":"2026-05-18T01:40:22.673098+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9509122v2","created_at":"2026-05-18T01:40:22.673098+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9509122","created_at":"2026-05-18T01:40:22.673098+00:00"},{"alias_kind":"pith_short_12","alias_value":"HSS2JMAUVEQ3","created_at":"2026-05-18T12:25:47.700082+00:00"},{"alias_kind":"pith_short_16","alias_value":"HSS2JMAUVEQ35ORH","created_at":"2026-05-18T12:25:47.700082+00:00"},{"alias_kind":"pith_short_8","alias_value":"HSS2JMAU","created_at":"2026-05-18T12:25:47.700082+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":9,"internal_anchor_count":6,"sample":[{"citing_arxiv_id":"2509.03458","citing_title":"Comparison of Halo Model and Simulation Predictions for Projected-Field Kinematic Sunyaev-Zel'dovich Cross-Correlations","ref_index":24,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21212","citing_title":"Detection of a dark matter subhalo in the strongly lensed system PJ011646","ref_index":103,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19121","citing_title":"Ringdown Signatures of Dehnen Dark Matter Halos: Fluid Modes and Detectability with Space-Based Detectors","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20117","citing_title":"The potential of diffuse Galactic Ridge neutrino measurements to constrain dark matter","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2605.16994","citing_title":"Determination of the best dark matter profile for the Milky Way with Gaia DR3 using Bayesian Model Comparison","ref_index":54,"is_internal_anchor":true},{"citing_arxiv_id":"2406.01705","citing_title":"Dark Matter","ref_index":10,"is_internal_anchor":true},{"citing_arxiv_id":"2605.03428","citing_title":"Families of regular spacetimes and energy conditions","ref_index":97,"is_internal_anchor":false},{"citing_arxiv_id":"2605.10857","citing_title":"Milky Way Dynamics Favor Dark Matter over Modified Gravity Models","ref_index":50,"is_internal_anchor":false},{"citing_arxiv_id":"2605.03428","citing_title":"Families of regular spacetimes and energy conditions","ref_index":100,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L","json":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L.json","graph_json":"https://pith.science/api/pith-number/HSS2JMAUVEQ35ORHBNBZZSEL6L/graph.json","events_json":"https://pith.science/api/pith-number/HSS2JMAUVEQ35ORHBNBZZSEL6L/events.json","paper":"https://pith.science/paper/HSS2JMAU"},"agent_actions":{"view_html":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L","download_json":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L.json","view_paper":"https://pith.science/paper/HSS2JMAU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9509122&json=true","fetch_graph":"https://pith.science/api/pith-number/HSS2JMAUVEQ35ORHBNBZZSEL6L/graph.json","fetch_events":"https://pith.science/api/pith-number/HSS2JMAUVEQ35ORHBNBZZSEL6L/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L/action/storage_attestation","attest_author":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L/action/author_attestation","sign_citation":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L/action/citation_signature","submit_replication":"https://pith.science/pith/HSS2JMAUVEQ35ORHBNBZZSEL6L/action/replication_record"}},"created_at":"2026-05-18T01:40:22.673098+00:00","updated_at":"2026-05-18T01:40:22.673098+00:00"}