{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:2LAF5KA36NGIF25TM3LZGDB5MQ","short_pith_number":"pith:2LAF5KA3","schema_version":"1.0","canonical_sha256":"d2c05ea81bf34c82ebb366d7930c3d6430b7997c4709df0bfe1f8ed9b64756ec","source":{"kind":"arxiv","id":"2302.05542","version":2},"attestation_state":"computed","paper":{"title":"Dynamics of intermediate mass black holes in globular clusters. Wander radius and anisotropy profiles","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Alessandro A. Trani, Luca Barbieri, Mario Pasquato, Pierfrancesco Di Cintio, Ugo N. di Carlo","submitted_at":"2023-02-10T23:09:34Z","abstract_excerpt":"We recently introduced a new method for simulating collisional gravitational N-body systems with approximately linear time scaling with $N$, based on the Multi-Particle Collision (MPC) scheme, previously applied in Plasma Physics. We simulate globular clusters with a realistic number of stellar particles (at least up to several times $10^6$) on a standard workstation. We simulate clusters hosting an intermediate mass black hole (IMBH), probing a broad range of BH-cluster and BH-average-star mass ratios, unrestricted by the computational constraints affecting direct N-body codes. We use either "},"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":"2302.05542","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-02-10T23:09:34Z","cross_cats_sorted":[],"title_canon_sha256":"16f5d31df033eac91c889d9c407e11a00e193101ac829a5ef48c4ec145677e0c","abstract_canon_sha256":"c3c3aa7336980d9d40335f548c872d4cf1f2cc6395f0e806d4d19caf5f3d2b6b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:04:30.394527Z","signature_b64":"yMn4OLhMAZcsi11NQyL/t12r9ADdegFT0JXFVlXDXGW4gAsSk2YYMWh8vi2PX7klYM23JK0xK/ayPKgpYAatBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d2c05ea81bf34c82ebb366d7930c3d6430b7997c4709df0bfe1f8ed9b64756ec","last_reissued_at":"2026-07-05T06:04:30.394061Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:04:30.394061Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dynamics of intermediate mass black holes in globular clusters. Wander radius and anisotropy profiles","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Alessandro A. Trani, Luca Barbieri, Mario Pasquato, Pierfrancesco Di Cintio, Ugo N. di Carlo","submitted_at":"2023-02-10T23:09:34Z","abstract_excerpt":"We recently introduced a new method for simulating collisional gravitational N-body systems with approximately linear time scaling with $N$, based on the Multi-Particle Collision (MPC) scheme, previously applied in Plasma Physics. We simulate globular clusters with a realistic number of stellar particles (at least up to several times $10^6$) on a standard workstation. We simulate clusters hosting an intermediate mass black hole (IMBH), probing a broad range of BH-cluster and BH-average-star mass ratios, unrestricted by the computational constraints affecting direct N-body codes. We use either "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2302.05542","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/2302.05542/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":"2302.05542","created_at":"2026-07-05T06:04:30.394117+00:00"},{"alias_kind":"arxiv_version","alias_value":"2302.05542v2","created_at":"2026-07-05T06:04:30.394117+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2302.05542","created_at":"2026-07-05T06:04:30.394117+00:00"},{"alias_kind":"pith_short_12","alias_value":"2LAF5KA36NGI","created_at":"2026-07-05T06:04:30.394117+00:00"},{"alias_kind":"pith_short_16","alias_value":"2LAF5KA36NGIF25T","created_at":"2026-07-05T06:04:30.394117+00:00"},{"alias_kind":"pith_short_8","alias_value":"2LAF5KA3","created_at":"2026-07-05T06:04:30.394117+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06154","citing_title":"Pulsars in Globular Clusters With the SKAO","ref_index":54,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ","json":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ.json","graph_json":"https://pith.science/api/pith-number/2LAF5KA36NGIF25TM3LZGDB5MQ/graph.json","events_json":"https://pith.science/api/pith-number/2LAF5KA36NGIF25TM3LZGDB5MQ/events.json","paper":"https://pith.science/paper/2LAF5KA3"},"agent_actions":{"view_html":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ","download_json":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ.json","view_paper":"https://pith.science/paper/2LAF5KA3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2302.05542&json=true","fetch_graph":"https://pith.science/api/pith-number/2LAF5KA36NGIF25TM3LZGDB5MQ/graph.json","fetch_events":"https://pith.science/api/pith-number/2LAF5KA36NGIF25TM3LZGDB5MQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ/action/storage_attestation","attest_author":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ/action/author_attestation","sign_citation":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ/action/citation_signature","submit_replication":"https://pith.science/pith/2LAF5KA36NGIF25TM3LZGDB5MQ/action/replication_record"}},"created_at":"2026-07-05T06:04:30.394117+00:00","updated_at":"2026-07-05T06:04:30.394117+00:00"}