{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:5UP2UI3GFJ5RXBPHMACFBUUO6H","short_pith_number":"pith:5UP2UI3G","schema_version":"1.0","canonical_sha256":"ed1faa23662a7b1b85e7600450d28ef1c95f735dee50c5e71d3bd46e8b0b4c5f","source":{"kind":"arxiv","id":"1907.04341","version":1},"attestation_state":"computed","paper":{"title":"Realistic sensitivity curves for pulsar timing arrays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"gr-qc","authors_text":"Jeffrey S. Hazboun, Joseph D. Romano, Tristan L. Smith","submitted_at":"2019-07-09T18:01:12Z","abstract_excerpt":"We construct realistic sensitivity curves for pulsar timing array searches for gravitational waves, incorporating both red and white noise contributions to individual pulsar noise spectra, as well as the effect of fitting to a pulsar timing model. We demonstrate the method on both simulated pulsars and a realistic array consisting of a subset of NANOGrav pulsars used in recent analyses. A comparison between the results presented here and exact sensitivity curves shows agreement to tens of percent. The resulting sensitivity curves can be used to assess the detectability of predicted 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":"1907.04341","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2019-07-09T18:01:12Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"af883dd43888a56c591fa17e9ee366ff4ee17c02f1c072fb658f83b532ae2837","abstract_canon_sha256":"f44c5c3ad8f89b76bcf3ef81b586b84b42bf527d79abe48e7149aa5a1fd4d628"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:20:17.029949Z","signature_b64":"XQPL4eOwEwvua9Vy5cHE6YAzibcURDdjqVmNVozF1V4GMa/WX/t8PYKS9puNRsskgbgDJW7jmU+f8JDW+VV4Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ed1faa23662a7b1b85e7600450d28ef1c95f735dee50c5e71d3bd46e8b0b4c5f","last_reissued_at":"2026-07-05T00:20:17.029546Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:20:17.029546Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Realistic sensitivity curves for pulsar timing arrays","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"gr-qc","authors_text":"Jeffrey S. Hazboun, Joseph D. Romano, Tristan L. Smith","submitted_at":"2019-07-09T18:01:12Z","abstract_excerpt":"We construct realistic sensitivity curves for pulsar timing array searches for gravitational waves, incorporating both red and white noise contributions to individual pulsar noise spectra, as well as the effect of fitting to a pulsar timing model. We demonstrate the method on both simulated pulsars and a realistic array consisting of a subset of NANOGrav pulsars used in recent analyses. A comparison between the results presented here and exact sensitivity curves shows agreement to tens of percent. The resulting sensitivity curves can be used to assess the detectability of predicted gravitation"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1907.04341","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/1907.04341/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":"1907.04341","created_at":"2026-07-05T00:20:17.029601+00:00"},{"alias_kind":"arxiv_version","alias_value":"1907.04341v1","created_at":"2026-07-05T00:20:17.029601+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1907.04341","created_at":"2026-07-05T00:20:17.029601+00:00"},{"alias_kind":"pith_short_12","alias_value":"5UP2UI3GFJ5R","created_at":"2026-07-05T00:20:17.029601+00:00"},{"alias_kind":"pith_short_16","alias_value":"5UP2UI3GFJ5RXBPH","created_at":"2026-07-05T00:20:17.029601+00:00"},{"alias_kind":"pith_short_8","alias_value":"5UP2UI3G","created_at":"2026-07-05T00:20:17.029601+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":0,"sample":[{"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":42,"is_internal_anchor":false},{"citing_arxiv_id":"2002.04615","citing_title":"New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions","ref_index":204,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22634","citing_title":"Constraints on the Primordial Black Hole Abundance using Pulsar Parameter Drifts","ref_index":56,"is_internal_anchor":false},{"citing_arxiv_id":"2604.21010","citing_title":"Gravity Echoes from Supermassive Black Hole Binaries","ref_index":34,"is_internal_anchor":false},{"citing_arxiv_id":"2604.20975","citing_title":"Probing Supermassive Black Hole Mergers with Pulsar Timing Arrays","ref_index":54,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08373","citing_title":"Stochastic problems in pulsar timing","ref_index":117,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H","json":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H.json","graph_json":"https://pith.science/api/pith-number/5UP2UI3GFJ5RXBPHMACFBUUO6H/graph.json","events_json":"https://pith.science/api/pith-number/5UP2UI3GFJ5RXBPHMACFBUUO6H/events.json","paper":"https://pith.science/paper/5UP2UI3G"},"agent_actions":{"view_html":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H","download_json":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H.json","view_paper":"https://pith.science/paper/5UP2UI3G","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1907.04341&json=true","fetch_graph":"https://pith.science/api/pith-number/5UP2UI3GFJ5RXBPHMACFBUUO6H/graph.json","fetch_events":"https://pith.science/api/pith-number/5UP2UI3GFJ5RXBPHMACFBUUO6H/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H/action/storage_attestation","attest_author":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H/action/author_attestation","sign_citation":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H/action/citation_signature","submit_replication":"https://pith.science/pith/5UP2UI3GFJ5RXBPHMACFBUUO6H/action/replication_record"}},"created_at":"2026-07-05T00:20:17.029601+00:00","updated_at":"2026-07-05T00:20:17.029601+00:00"}