{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:I2VHS3IGKFANXKOWUH4HVTSHNR","short_pith_number":"pith:I2VHS3IG","schema_version":"1.0","canonical_sha256":"46aa796d065140dba9d6a1f87ace476c5693dd3248f1c89307f4f18c8e7244f4","source":{"kind":"arxiv","id":"astro-ph/0406231","version":1},"attestation_state":"computed","paper":{"title":"Massive Black Holes in Star Clusters. II. Realistic Cluster Models","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Holger Baumgardt, Junichiro Makino, Toshikazu Ebisuzaki","submitted_at":"2004-06-09T14:02:59Z","abstract_excerpt":"We have followed the evolution of multi-mass star clusters containing massive central black holes through collisional N-body simulations done on GRAPE6. Each cluster is composed of between 16,384 to 131,072 stars together with a black hole with an initial mass of M_BH=1000 Msun. We follow the evolution of the clusters under the combined influence of two-body relaxation, stellar mass-loss and tidal disruption of stars.\n  The (3D) mass density profile follows a power-law distribution \\rho \\sim r^{-\\alpha} with slope \\alpha=1.55. This leads to a constant density profile of bright stars in project"},"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/0406231","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-06-09T14:02:59Z","cross_cats_sorted":[],"title_canon_sha256":"af8a4bfe47908c7fae097136f17c7b12c477db6e4a3d345b29faccd69530cc52","abstract_canon_sha256":"4dc26af19721c4539bf0a8b871d71971c6ebdbc8a62b21847d844e013b3d725d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:43:58.425145Z","signature_b64":"Hja4Aco3GwIk+0lFXpgsdW5TjJasjIf0EoZeooR6RlTse90SgxsCh66WowKMIVNTgLzfM6xszIX2rqyKDQl/Ag==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"46aa796d065140dba9d6a1f87ace476c5693dd3248f1c89307f4f18c8e7244f4","last_reissued_at":"2026-07-04T16:43:58.424740Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:43:58.424740Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Massive Black Holes in Star Clusters. II. Realistic Cluster Models","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Holger Baumgardt, Junichiro Makino, Toshikazu Ebisuzaki","submitted_at":"2004-06-09T14:02:59Z","abstract_excerpt":"We have followed the evolution of multi-mass star clusters containing massive central black holes through collisional N-body simulations done on GRAPE6. Each cluster is composed of between 16,384 to 131,072 stars together with a black hole with an initial mass of M_BH=1000 Msun. We follow the evolution of the clusters under the combined influence of two-body relaxation, stellar mass-loss and tidal disruption of stars.\n  The (3D) mass density profile follows a power-law distribution \\rho \\sim r^{-\\alpha} with slope \\alpha=1.55. This leads to a constant density profile of bright stars in project"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0406231","kind":"arxiv","version":1},"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/0406231/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/0406231","created_at":"2026-07-04T16:43:58.424803+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0406231v1","created_at":"2026-07-04T16:43:58.424803+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0406231","created_at":"2026-07-04T16:43:58.424803+00:00"},{"alias_kind":"pith_short_12","alias_value":"I2VHS3IGKFAN","created_at":"2026-07-04T16:43:58.424803+00:00"},{"alias_kind":"pith_short_16","alias_value":"I2VHS3IGKFANXKOW","created_at":"2026-07-04T16:43:58.424803+00:00"},{"alias_kind":"pith_short_8","alias_value":"I2VHS3IG","created_at":"2026-07-04T16:43:58.424803+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.08201","citing_title":"Detecting Intermediate-mass Black Holes Using Miniature Pulsar Timing Arrays in Globular Clusters","ref_index":25,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR","json":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR.json","graph_json":"https://pith.science/api/pith-number/I2VHS3IGKFANXKOWUH4HVTSHNR/graph.json","events_json":"https://pith.science/api/pith-number/I2VHS3IGKFANXKOWUH4HVTSHNR/events.json","paper":"https://pith.science/paper/I2VHS3IG"},"agent_actions":{"view_html":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR","download_json":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR.json","view_paper":"https://pith.science/paper/I2VHS3IG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0406231&json=true","fetch_graph":"https://pith.science/api/pith-number/I2VHS3IGKFANXKOWUH4HVTSHNR/graph.json","fetch_events":"https://pith.science/api/pith-number/I2VHS3IGKFANXKOWUH4HVTSHNR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR/action/storage_attestation","attest_author":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR/action/author_attestation","sign_citation":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR/action/citation_signature","submit_replication":"https://pith.science/pith/I2VHS3IGKFANXKOWUH4HVTSHNR/action/replication_record"}},"created_at":"2026-07-04T16:43:58.424803+00:00","updated_at":"2026-07-04T16:43:58.424803+00:00"}