{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:S327MBUUCRFPUCRC2KFXZCBQ3I","short_pith_number":"pith:S327MBUU","schema_version":"1.0","canonical_sha256":"96f5f60694144afa0a22d28b7c8830da385d5099095630b62e510b916224ee07","source":{"kind":"arxiv","id":"2408.10139","version":2},"attestation_state":"computed","paper":{"title":"Characterizing the nanohertz gravitational wave background using a $t$-process power spectral density","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.HE","authors_text":"Joseph Simon, Sarah J. Vigeland, Shashwat C. Sardesai","submitted_at":"2024-08-19T16:40:15Z","abstract_excerpt":"Pulsar timing arrays are sensitive to low-frequency gravitational waves (GWs), which induce correlated changes in millisecond pulsars' timing residuals. PTA collaborations around the world have recently announced evidence of a nanohertz gravitational wave background (GWB), which may be produced by a population of supermassive black hole binaries (SMBHBs). The GWB is often modeled as following a power-law power spectral density (PSD); however, a GWB produced by a cosmological population of SMBHBs is expected to have a more complex power spectrum due to the discrete nature of the sources. In thi"},"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":"2408.10139","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-08-19T16:40:15Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"3809bb85609a1ff0e01a45e1f5642753353bb153936dac001bd19979142ba87b","abstract_canon_sha256":"577b1b54a52925b65ba3c4bcae373ebf4e15c206ab988ada95eb19a225380d7b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:24:17.826058Z","signature_b64":"wm84D6YqZsrdLZM3NMsOPU8ttq4wZQ/zadm3fMa5EGeZN8zN+xAuEfExq/CO0LU3c3aIRyZccopNPgaTMWWyDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"96f5f60694144afa0a22d28b7c8830da385d5099095630b62e510b916224ee07","last_reissued_at":"2026-07-05T09:24:17.825537Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:24:17.825537Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Characterizing the nanohertz gravitational wave background using a $t$-process power spectral density","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.HE","authors_text":"Joseph Simon, Sarah J. Vigeland, Shashwat C. Sardesai","submitted_at":"2024-08-19T16:40:15Z","abstract_excerpt":"Pulsar timing arrays are sensitive to low-frequency gravitational waves (GWs), which induce correlated changes in millisecond pulsars' timing residuals. PTA collaborations around the world have recently announced evidence of a nanohertz gravitational wave background (GWB), which may be produced by a population of supermassive black hole binaries (SMBHBs). The GWB is often modeled as following a power-law power spectral density (PSD); however, a GWB produced by a cosmological population of SMBHBs is expected to have a more complex power spectrum due to the discrete nature of the sources. In thi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2408.10139","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/2408.10139/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":"2408.10139","created_at":"2026-07-05T09:24:17.825595+00:00"},{"alias_kind":"arxiv_version","alias_value":"2408.10139v2","created_at":"2026-07-05T09:24:17.825595+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2408.10139","created_at":"2026-07-05T09:24:17.825595+00:00"},{"alias_kind":"pith_short_12","alias_value":"S327MBUUCRFP","created_at":"2026-07-05T09:24:17.825595+00:00"},{"alias_kind":"pith_short_16","alias_value":"S327MBUUCRFPUCRC","created_at":"2026-07-05T09:24:17.825595+00:00"},{"alias_kind":"pith_short_8","alias_value":"S327MBUU","created_at":"2026-07-05T09:24:17.825595+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07477","citing_title":"Population statistics of nanohertz gravitational wave sources","ref_index":42,"is_internal_anchor":true},{"citing_arxiv_id":"2606.18241","citing_title":"A Joint Optimal Search for Gravitational Waves from Resolved and Unresolved Supermassive Binary Black Holes with Pulsar Timing Arrays","ref_index":32,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I","json":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I.json","graph_json":"https://pith.science/api/pith-number/S327MBUUCRFPUCRC2KFXZCBQ3I/graph.json","events_json":"https://pith.science/api/pith-number/S327MBUUCRFPUCRC2KFXZCBQ3I/events.json","paper":"https://pith.science/paper/S327MBUU"},"agent_actions":{"view_html":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I","download_json":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I.json","view_paper":"https://pith.science/paper/S327MBUU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2408.10139&json=true","fetch_graph":"https://pith.science/api/pith-number/S327MBUUCRFPUCRC2KFXZCBQ3I/graph.json","fetch_events":"https://pith.science/api/pith-number/S327MBUUCRFPUCRC2KFXZCBQ3I/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I/action/timestamp_anchor","attest_storage":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I/action/storage_attestation","attest_author":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I/action/author_attestation","sign_citation":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I/action/citation_signature","submit_replication":"https://pith.science/pith/S327MBUUCRFPUCRC2KFXZCBQ3I/action/replication_record"}},"created_at":"2026-07-05T09:24:17.825595+00:00","updated_at":"2026-07-05T09:24:17.825595+00:00"}