{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:W2XXS4CGRI4DTO3FD6FGUORVLR","short_pith_number":"pith:W2XXS4CG","schema_version":"1.0","canonical_sha256":"b6af7970468a3839bb651f8a6a3a355c74ad06064e325cda93a0767b9f95e727","source":{"kind":"arxiv","id":"1811.05003","version":1},"attestation_state":"computed","paper":{"title":"On the detectability of ultralight scalar field dark matter with gravitational-wave detectors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-ph","authors_text":"Soichiro Morisaki, Teruaki Suyama","submitted_at":"2018-11-09T13:38:59Z","abstract_excerpt":"An ultralight scalar field is one of the dark matter candidates. If it couples with Standard Model particles, it oscillates mirrors in gravitational-wave detectors and generates detectable signals. We study the spectra of the signals taking into account the motion of the detectors due to the Earth's rotation/the detectors' orbital motion around the Sun and formulate a suitable data-analysis method to detect it. We find that our method can improve the existing constraints given by fifth-force experiments on one of the scalar field's coupling constants by a factor of $\\sim 30$, $\\sim 100$ and $\\"},"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":"1811.05003","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2018-11-09T13:38:59Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"54e2dbfc4d8dc1109bed7ca8f41bf005803e4d661473ca5f8b2b78ea0a718c15","abstract_canon_sha256":"83aa31cf1471866e21f7ea9a8128833f557aacff4841555d2803613fe68cf668"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:26:32.755490Z","signature_b64":"ZRgnM+zjzWU2KIjst5UcAys5DdqdSo6rIEXYnzsmy8WzjBKAXpysbvDP6+Q1r1sGtUJyPZ2cvE/d1zBTfXN3AQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b6af7970468a3839bb651f8a6a3a355c74ad06064e325cda93a0767b9f95e727","last_reissued_at":"2026-07-05T00:26:32.755020Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:26:32.755020Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the detectability of ultralight scalar field dark matter with gravitational-wave detectors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-ph","authors_text":"Soichiro Morisaki, Teruaki Suyama","submitted_at":"2018-11-09T13:38:59Z","abstract_excerpt":"An ultralight scalar field is one of the dark matter candidates. If it couples with Standard Model particles, it oscillates mirrors in gravitational-wave detectors and generates detectable signals. We study the spectra of the signals taking into account the motion of the detectors due to the Earth's rotation/the detectors' orbital motion around the Sun and formulate a suitable data-analysis method to detect it. We find that our method can improve the existing constraints given by fifth-force experiments on one of the scalar field's coupling constants by a factor of $\\sim 30$, $\\sim 100$ and $\\"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1811.05003","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/1811.05003/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":"1811.05003","created_at":"2026-07-05T00:26:32.755077+00:00"},{"alias_kind":"arxiv_version","alias_value":"1811.05003v1","created_at":"2026-07-05T00:26:32.755077+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1811.05003","created_at":"2026-07-05T00:26:32.755077+00:00"},{"alias_kind":"pith_short_12","alias_value":"W2XXS4CGRI4D","created_at":"2026-07-05T00:26:32.755077+00:00"},{"alias_kind":"pith_short_16","alias_value":"W2XXS4CGRI4DTO3F","created_at":"2026-07-05T00:26:32.755077+00:00"},{"alias_kind":"pith_short_8","alias_value":"W2XXS4CG","created_at":"2026-07-05T00:26:32.755077+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08248","citing_title":"Probing Quadratically Coupled Ultralight Dark Matter with the Laser Interferometer Space Antenna","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2606.03478","citing_title":"Signatures of Ultralight Dark Matter in Space-Based Laser Interferometers","ref_index":29,"is_internal_anchor":false},{"citing_arxiv_id":"2606.28071","citing_title":"Construction of Sensitivity Curves for Dynamic LISA and Taiji","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2507.15951","citing_title":"Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter","ref_index":45,"is_internal_anchor":false},{"citing_arxiv_id":"2604.23879","citing_title":"Searching for ultralight bosons with Josephson junction interferometry","ref_index":1,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR","json":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR.json","graph_json":"https://pith.science/api/pith-number/W2XXS4CGRI4DTO3FD6FGUORVLR/graph.json","events_json":"https://pith.science/api/pith-number/W2XXS4CGRI4DTO3FD6FGUORVLR/events.json","paper":"https://pith.science/paper/W2XXS4CG"},"agent_actions":{"view_html":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR","download_json":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR.json","view_paper":"https://pith.science/paper/W2XXS4CG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1811.05003&json=true","fetch_graph":"https://pith.science/api/pith-number/W2XXS4CGRI4DTO3FD6FGUORVLR/graph.json","fetch_events":"https://pith.science/api/pith-number/W2XXS4CGRI4DTO3FD6FGUORVLR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR/action/storage_attestation","attest_author":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR/action/author_attestation","sign_citation":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR/action/citation_signature","submit_replication":"https://pith.science/pith/W2XXS4CGRI4DTO3FD6FGUORVLR/action/replication_record"}},"created_at":"2026-07-05T00:26:32.755077+00:00","updated_at":"2026-07-05T00:26:32.755077+00:00"}