{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:NJWXLLSUMJJ6TIGTQPNGKQZ4BP","short_pith_number":"pith:NJWXLLSU","schema_version":"1.0","canonical_sha256":"6a6d75ae546253e9a0d383da65433c0bd9a47bbaa7999af7e25942689873b0ef","source":{"kind":"arxiv","id":"0809.3412","version":2},"attestation_state":"computed","paper":{"title":"Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"A. Sesana, A. Vecchio, M. Volonteri","submitted_at":"2008-09-19T16:32:17Z","abstract_excerpt":"Massive black holes are key components of the assembly and evolution of cosmic structures and a number of surveys are currently on-going or planned to probe the demographics of these objects and to gain insight into the relevant physical processes. Pulsar Timing Arrays (PTAs) currently provide the only means to observe gravitational radiation from massive black hole binary systems with masses >10^7 solar masses. The whole cosmic population produces a stochastic background that could be detectable with upcoming Pulsar Timing Arrays. Sources sufficiently close and/or massive generate gravitation"},"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":"0809.3412","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-09-19T16:32:17Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"cd75230766e633bb17d86d3dff2120d44bf2052a00eeca34ec845827ce993b25","abstract_canon_sha256":"227acef2d1ec013bb0810e1795beecb1822f6509a24036e9c0d79584124d9ab4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:12:54.250124Z","signature_b64":"cgDMAx70zZrbCZHxDh/6wQL5tnh970gEjnRJNFilVDlPNL599XUsKT3wGlLkkuuej7uklkd+rNGxfReJnPrIAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6a6d75ae546253e9a0d383da65433c0bd9a47bbaa7999af7e25942689873b0ef","last_reissued_at":"2026-07-04T17:12:54.249782Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:12:54.249782Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gravitational waves from resolvable massive black hole binary systems and observations with Pulsar Timing Arrays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"A. Sesana, A. Vecchio, M. Volonteri","submitted_at":"2008-09-19T16:32:17Z","abstract_excerpt":"Massive black holes are key components of the assembly and evolution of cosmic structures and a number of surveys are currently on-going or planned to probe the demographics of these objects and to gain insight into the relevant physical processes. Pulsar Timing Arrays (PTAs) currently provide the only means to observe gravitational radiation from massive black hole binary systems with masses >10^7 solar masses. The whole cosmic population produces a stochastic background that could be detectable with upcoming Pulsar Timing Arrays. Sources sufficiently close and/or massive generate gravitation"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0809.3412","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/0809.3412/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":"0809.3412","created_at":"2026-07-04T17:12:54.249835+00:00"},{"alias_kind":"arxiv_version","alias_value":"0809.3412v2","created_at":"2026-07-04T17:12:54.249835+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0809.3412","created_at":"2026-07-04T17:12:54.249835+00:00"},{"alias_kind":"pith_short_12","alias_value":"NJWXLLSUMJJ6","created_at":"2026-07-04T17:12:54.249835+00:00"},{"alias_kind":"pith_short_16","alias_value":"NJWXLLSUMJJ6TIGT","created_at":"2026-07-04T17:12:54.249835+00:00"},{"alias_kind":"pith_short_8","alias_value":"NJWXLLSU","created_at":"2026-07-04T17:12:54.249835+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2607.07477","citing_title":"Population statistics of nanohertz gravitational wave sources","ref_index":69,"is_internal_anchor":true},{"citing_arxiv_id":"2606.00577","citing_title":"Searching for a waveform-agnostic gravitational wave signal in pulsar timing arrays","ref_index":14,"is_internal_anchor":true},{"citing_arxiv_id":"2510.01316","citing_title":"Expectations for the first supermassive black-hole binary resolved by PTAs II: Milestones for binary characterization","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2604.20975","citing_title":"Probing Supermassive Black Hole Mergers with Pulsar Timing Arrays","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08506","citing_title":"The Heavy Tailed Non-Gaussianity of the Supermassive Black Hole Gravitational Wave Background","ref_index":25,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP","json":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP.json","graph_json":"https://pith.science/api/pith-number/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/graph.json","events_json":"https://pith.science/api/pith-number/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/events.json","paper":"https://pith.science/paper/NJWXLLSU"},"agent_actions":{"view_html":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP","download_json":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP.json","view_paper":"https://pith.science/paper/NJWXLLSU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0809.3412&json=true","fetch_graph":"https://pith.science/api/pith-number/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/graph.json","fetch_events":"https://pith.science/api/pith-number/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/action/storage_attestation","attest_author":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/action/author_attestation","sign_citation":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/action/citation_signature","submit_replication":"https://pith.science/pith/NJWXLLSUMJJ6TIGTQPNGKQZ4BP/action/replication_record"}},"created_at":"2026-07-04T17:12:54.249835+00:00","updated_at":"2026-07-04T17:12:54.249835+00:00"}