{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:OVV55G7ZCQNXQRC3EU7ZWDZIY4","short_pith_number":"pith:OVV55G7Z","schema_version":"1.0","canonical_sha256":"756bde9bf9141b78445b253f9b0f28c734a7a252c57ebed774921ab824aba700","source":{"kind":"arxiv","id":"1705.04733","version":2},"attestation_state":"computed","paper":{"title":"Sensitivity of new detection method for ultra-low frequency gravitational waves with pulsar spin-down rate statistics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Hiroki Kumamoto, Keitaro Takahashi, Naoyuki Yonemaru, Sachiko Kuroyanagi","submitted_at":"2017-05-10T12:49:25Z","abstract_excerpt":"A new detection method for ultra-low frequency gravitational waves (GWs) with a frequency much lower than the observational range of pulsar timing arrays (PTAs) was suggested in Yonemaru et al. (2016). In the PTA analysis, ultra-low frequency GWs ($\\lesssim 10^{-10}$ Hz) which evolve just linearly during the observation time span are absorbed by the pulsar spin-down rates since both have the same effect on the pulse arrival time. Therefore, such GWs cannot be detected by the conventional method of PTAs. However, the bias on the observed spin-down rates depends on relative direction of a pulsar"},"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":"1705.04733","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2017-05-10T12:49:25Z","cross_cats_sorted":[],"title_canon_sha256":"69d5fe249e397d5ba14f9209e49ed4d4da9bbd69d7517d240d212686a7a0cd24","abstract_canon_sha256":"f3aca40f18aa5b2a14c049274d9989ac847c118cb7c904fbba82c6e778d677ff"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:17:09.324865Z","signature_b64":"urW2rMvVGwcc6J8cxH3mcdm0zIFeKuTyfxkXR3G7DmBqS7ScD6x6L/KyRs7LvxDbquTp1UztWvYgoQQETricAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"756bde9bf9141b78445b253f9b0f28c734a7a252c57ebed774921ab824aba700","last_reissued_at":"2026-05-18T00:17:09.324223Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:17:09.324223Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Sensitivity of new detection method for ultra-low frequency gravitational waves with pulsar spin-down rate statistics","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Hiroki Kumamoto, Keitaro Takahashi, Naoyuki Yonemaru, Sachiko Kuroyanagi","submitted_at":"2017-05-10T12:49:25Z","abstract_excerpt":"A new detection method for ultra-low frequency gravitational waves (GWs) with a frequency much lower than the observational range of pulsar timing arrays (PTAs) was suggested in Yonemaru et al. (2016). In the PTA analysis, ultra-low frequency GWs ($\\lesssim 10^{-10}$ Hz) which evolve just linearly during the observation time span are absorbed by the pulsar spin-down rates since both have the same effect on the pulse arrival time. Therefore, such GWs cannot be detected by the conventional method of PTAs. However, the bias on the observed spin-down rates depends on relative direction of a pulsar"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1705.04733","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":""},"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":"1705.04733","created_at":"2026-05-18T00:17:09.324332+00:00"},{"alias_kind":"arxiv_version","alias_value":"1705.04733v2","created_at":"2026-05-18T00:17:09.324332+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1705.04733","created_at":"2026-05-18T00:17:09.324332+00:00"},{"alias_kind":"pith_short_12","alias_value":"OVV55G7ZCQNX","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_16","alias_value":"OVV55G7ZCQNXQRC3","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_8","alias_value":"OVV55G7Z","created_at":"2026-05-18T12:31:34.259226+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.18085","citing_title":"First astrometric constraints on parity-violation in the gravitational wave background","ref_index":42,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4","json":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4.json","graph_json":"https://pith.science/api/pith-number/OVV55G7ZCQNXQRC3EU7ZWDZIY4/graph.json","events_json":"https://pith.science/api/pith-number/OVV55G7ZCQNXQRC3EU7ZWDZIY4/events.json","paper":"https://pith.science/paper/OVV55G7Z"},"agent_actions":{"view_html":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4","download_json":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4.json","view_paper":"https://pith.science/paper/OVV55G7Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1705.04733&json=true","fetch_graph":"https://pith.science/api/pith-number/OVV55G7ZCQNXQRC3EU7ZWDZIY4/graph.json","fetch_events":"https://pith.science/api/pith-number/OVV55G7ZCQNXQRC3EU7ZWDZIY4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4/action/storage_attestation","attest_author":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4/action/author_attestation","sign_citation":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4/action/citation_signature","submit_replication":"https://pith.science/pith/OVV55G7ZCQNXQRC3EU7ZWDZIY4/action/replication_record"}},"created_at":"2026-05-18T00:17:09.324332+00:00","updated_at":"2026-05-18T00:17:09.324332+00:00"}