{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:R7FD37ZCXHYYHG4MHSKUTE6CXK","short_pith_number":"pith:R7FD37ZC","schema_version":"1.0","canonical_sha256":"8fca3dff22b9f1839b8c3c954993c2bab65756ace3035b2d9613527170be432c","source":{"kind":"arxiv","id":"2303.02834","version":1},"attestation_state":"computed","paper":{"title":"Timing of Pulsars in the Globular Cluster Omega Centauri","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"B. Bhattacharyya, E. Keane, F. Camilo, J. Berteaud, M. Kerr, S. Dai, S. Johnston","submitted_at":"2023-03-06T02:01:11Z","abstract_excerpt":"We present the timing of the first five millisecond pulsars discovered in the globular cluster Omega Centauri and the discovery of a pulsar with a spin period of 3.68 ms. With a timing baseline of $\\sim$3.5 yr we are able to measure the derivative of the spin frequency ($\\dot{\\nu}$) for the first five pulsars. Upper limits on the pulsar line-of-sight acceleration are estimated and compared with predictions based on analytical models of the cluster. We find that PSRs J1326$-$4728B and D show large negative accelerations, which are in tension with the minimum acceleration predicted by analytical"},"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":"2303.02834","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-03-06T02:01:11Z","cross_cats_sorted":[],"title_canon_sha256":"c0d0919c1b021184fc0a7d1bd0a7b11722e706cdacde3ec3f99b10f02561a00d","abstract_canon_sha256":"f3d8ddb7b1116bf2c72d74c13dd5b1844c814101a9aacd7736b414c77e6ea8da"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:55:52.755842Z","signature_b64":"xWLodTmqM1QAf2pNsA0hVedN5sfpODUEjb1hUNXcpxlaGeQ/vgzXJO2JfvFATHRRpu7xWjxB3ACp884AL0DcDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8fca3dff22b9f1839b8c3c954993c2bab65756ace3035b2d9613527170be432c","last_reissued_at":"2026-07-05T05:55:52.755350Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:55:52.755350Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Timing of Pulsars in the Globular Cluster Omega Centauri","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"B. Bhattacharyya, E. Keane, F. Camilo, J. Berteaud, M. Kerr, S. Dai, S. Johnston","submitted_at":"2023-03-06T02:01:11Z","abstract_excerpt":"We present the timing of the first five millisecond pulsars discovered in the globular cluster Omega Centauri and the discovery of a pulsar with a spin period of 3.68 ms. With a timing baseline of $\\sim$3.5 yr we are able to measure the derivative of the spin frequency ($\\dot{\\nu}$) for the first five pulsars. Upper limits on the pulsar line-of-sight acceleration are estimated and compared with predictions based on analytical models of the cluster. We find that PSRs J1326$-$4728B and D show large negative accelerations, which are in tension with the minimum acceleration predicted by analytical"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2303.02834","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/2303.02834/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":"2303.02834","created_at":"2026-07-05T05:55:52.755411+00:00"},{"alias_kind":"arxiv_version","alias_value":"2303.02834v1","created_at":"2026-07-05T05:55:52.755411+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2303.02834","created_at":"2026-07-05T05:55:52.755411+00:00"},{"alias_kind":"pith_short_12","alias_value":"R7FD37ZCXHYY","created_at":"2026-07-05T05:55:52.755411+00:00"},{"alias_kind":"pith_short_16","alias_value":"R7FD37ZCXHYYHG4M","created_at":"2026-07-05T05:55:52.755411+00:00"},{"alias_kind":"pith_short_8","alias_value":"R7FD37ZC","created_at":"2026-07-05T05:55:52.755411+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":20,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK","json":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK.json","graph_json":"https://pith.science/api/pith-number/R7FD37ZCXHYYHG4MHSKUTE6CXK/graph.json","events_json":"https://pith.science/api/pith-number/R7FD37ZCXHYYHG4MHSKUTE6CXK/events.json","paper":"https://pith.science/paper/R7FD37ZC"},"agent_actions":{"view_html":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK","download_json":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK.json","view_paper":"https://pith.science/paper/R7FD37ZC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2303.02834&json=true","fetch_graph":"https://pith.science/api/pith-number/R7FD37ZCXHYYHG4MHSKUTE6CXK/graph.json","fetch_events":"https://pith.science/api/pith-number/R7FD37ZCXHYYHG4MHSKUTE6CXK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK/action/storage_attestation","attest_author":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK/action/author_attestation","sign_citation":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK/action/citation_signature","submit_replication":"https://pith.science/pith/R7FD37ZCXHYYHG4MHSKUTE6CXK/action/replication_record"}},"created_at":"2026-07-05T05:55:52.755411+00:00","updated_at":"2026-07-05T05:55:52.755411+00:00"}