{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:KXHPRAJE3QKF4G2HMOJ3GKQEAJ","short_pith_number":"pith:KXHPRAJE","schema_version":"1.0","canonical_sha256":"55cef88124dc145e1b476393b32a04024381c92b00a8b671815c33f3a8cb4fec","source":{"kind":"arxiv","id":"1406.1369","version":2},"attestation_state":"computed","paper":{"title":"Implications of the B-mode Polarization Measurement for Direct Detection of Inflationary Gravitational Waves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Naoshi Sugiyama, Sachiko Kuroyanagi, Shinji Tsujikawa, Takeshi Chiba","submitted_at":"2014-06-05T12:57:39Z","abstract_excerpt":"The prospects for direct measurements of inflationary gravitational waves by next generation interferometric detectors inferred from the possible detection of B-mode polarization of the cosmic microwave background are studied. We compute the spectra of the gravitational wave background and the signal-to-noise ratios by two interferometric detectors (DECIGO and BBO) for large-field inflationary models in which the tensor-to-scalar ratio is greater than the order of 0.01. If the reheating temperature $T_{\\rm RH}$ of chaotic inflation with the quadratic potential is high ($T_{\\rm RH}>7.9\\times10^"},"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":"1406.1369","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-06-05T12:57:39Z","cross_cats_sorted":["gr-qc","hep-ph","hep-th"],"title_canon_sha256":"0f121a0d22a541a8e34ca23632c7a5a63f0aaee0f8bad8e5952adf6b4a793012","abstract_canon_sha256":"c3f8c8beb65328b8aee1b77fad1665022c6368b03f6ad9e9fbc08f9bbf8e5e60"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:40:47.126420Z","signature_b64":"ne6A78pLDt5c1k2HMlzWoir17BmzVVcyssFt4JEFg/u/eaxYpvOvpbjqQ246H9IPe1dwR39dICLKjNU/pJdbDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"55cef88124dc145e1b476393b32a04024381c92b00a8b671815c33f3a8cb4fec","last_reissued_at":"2026-05-18T02:40:47.125923Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:40:47.125923Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Implications of the B-mode Polarization Measurement for Direct Detection of Inflationary Gravitational Waves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Naoshi Sugiyama, Sachiko Kuroyanagi, Shinji Tsujikawa, Takeshi Chiba","submitted_at":"2014-06-05T12:57:39Z","abstract_excerpt":"The prospects for direct measurements of inflationary gravitational waves by next generation interferometric detectors inferred from the possible detection of B-mode polarization of the cosmic microwave background are studied. We compute the spectra of the gravitational wave background and the signal-to-noise ratios by two interferometric detectors (DECIGO and BBO) for large-field inflationary models in which the tensor-to-scalar ratio is greater than the order of 0.01. If the reheating temperature $T_{\\rm RH}$ of chaotic inflation with the quadratic potential is high ($T_{\\rm RH}>7.9\\times10^"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1406.1369","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":"1406.1369","created_at":"2026-05-18T02:40:47.125994+00:00"},{"alias_kind":"arxiv_version","alias_value":"1406.1369v2","created_at":"2026-05-18T02:40:47.125994+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1406.1369","created_at":"2026-05-18T02:40:47.125994+00:00"},{"alias_kind":"pith_short_12","alias_value":"KXHPRAJE3QKF","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_16","alias_value":"KXHPRAJE3QKF4G2H","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_8","alias_value":"KXHPRAJE","created_at":"2026-05-18T12:28:35.611951+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.26251","citing_title":"Supercool with PPO: Exploring Supercooled Phase Transitions via Reinforcement Learning","ref_index":80,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ","json":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ.json","graph_json":"https://pith.science/api/pith-number/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/graph.json","events_json":"https://pith.science/api/pith-number/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/events.json","paper":"https://pith.science/paper/KXHPRAJE"},"agent_actions":{"view_html":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ","download_json":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ.json","view_paper":"https://pith.science/paper/KXHPRAJE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1406.1369&json=true","fetch_graph":"https://pith.science/api/pith-number/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/graph.json","fetch_events":"https://pith.science/api/pith-number/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/action/storage_attestation","attest_author":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/action/author_attestation","sign_citation":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/action/citation_signature","submit_replication":"https://pith.science/pith/KXHPRAJE3QKF4G2HMOJ3GKQEAJ/action/replication_record"}},"created_at":"2026-05-18T02:40:47.125994+00:00","updated_at":"2026-05-18T02:40:47.125994+00:00"}