{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:NXALNWLRI3IRNDEGSWNWNZE4OI","short_pith_number":"pith:NXALNWLR","schema_version":"1.0","canonical_sha256":"6dc0b6d97146d1168c86959b66e49c722e82ea87195a2d75cd26bce81320e2bb","source":{"kind":"arxiv","id":"1410.6618","version":2},"attestation_state":"computed","paper":{"title":"Prospects of determination of reheating temperature after inflation by DECIGO","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":"Jun'ichi Yokoyama, Kazunori Nakayama, Sachiko Kuroyanagi","submitted_at":"2014-10-24T08:39:12Z","abstract_excerpt":"If the tensor-to-scalar ratio $r$ of cosmological perturbations takes a large value $r\\sim 0.1$, which may be inferred by recent BICEP2 result, we can hope to determine thermal history, in particular, the reheating temperature, $T_R$, after inflation by space-based laser interferometers. It is shown that upgraded and upshifted versions of DECIGO may be able to determine $T_R$ if it lies in the range $6\\times 10^6< T_R < 5\\times 10^7$GeV and $3\\times 10^7<T_R<2\\times 10^8$GeV, respectively. Although these ranges include predictions of some currently plausible inflation models, since each specif"},"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":"1410.6618","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-10-24T08:39:12Z","cross_cats_sorted":["gr-qc","hep-ph","hep-th"],"title_canon_sha256":"e7249a0987f3aed6179946cb8cc0df5edbee5a48b1150952acb4df467a7b9e45","abstract_canon_sha256":"d3c04e7b57ac1f57a9e2d66851cb8cf1e29a3ca971c6eee7df49f3f7f0155cbb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:26:45.204801Z","signature_b64":"mufKKlqUOMINOkzsQQowF3yAK3QfmXxML32H7gtn+5+rCcna1M4V98qvSQ1ORHegbmYJNhOnUThVd61dIPg3Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6dc0b6d97146d1168c86959b66e49c722e82ea87195a2d75cd26bce81320e2bb","last_reissued_at":"2026-05-18T02:26:45.204443Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:26:45.204443Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Prospects of determination of reheating temperature after inflation by DECIGO","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":"Jun'ichi Yokoyama, Kazunori Nakayama, Sachiko Kuroyanagi","submitted_at":"2014-10-24T08:39:12Z","abstract_excerpt":"If the tensor-to-scalar ratio $r$ of cosmological perturbations takes a large value $r\\sim 0.1$, which may be inferred by recent BICEP2 result, we can hope to determine thermal history, in particular, the reheating temperature, $T_R$, after inflation by space-based laser interferometers. It is shown that upgraded and upshifted versions of DECIGO may be able to determine $T_R$ if it lies in the range $6\\times 10^6< T_R < 5\\times 10^7$GeV and $3\\times 10^7<T_R<2\\times 10^8$GeV, respectively. Although these ranges include predictions of some currently plausible inflation models, since each specif"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.6618","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":"1410.6618","created_at":"2026-05-18T02:26:45.204498+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.6618v2","created_at":"2026-05-18T02:26:45.204498+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.6618","created_at":"2026-05-18T02:26:45.204498+00:00"},{"alias_kind":"pith_short_12","alias_value":"NXALNWLRI3IR","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_16","alias_value":"NXALNWLRI3IRNDEG","created_at":"2026-05-18T12:28:41.024544+00:00"},{"alias_kind":"pith_short_8","alias_value":"NXALNWLR","created_at":"2026-05-18T12:28:41.024544+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2002.04615","citing_title":"New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions","ref_index":200,"is_internal_anchor":true},{"citing_arxiv_id":"2511.02184","citing_title":"Dark Matter Freeze-in from a $Z^\\prime$ Reheaton","ref_index":20,"is_internal_anchor":true},{"citing_arxiv_id":"2601.00378","citing_title":"High Frequency Spectrum of Primordial Gravitational Waves","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2605.00735","citing_title":"DESI and Gravitational Wave Constraints Challenge Quintessential {\\alpha}-Attractor Inflation","ref_index":76,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI","json":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI.json","graph_json":"https://pith.science/api/pith-number/NXALNWLRI3IRNDEGSWNWNZE4OI/graph.json","events_json":"https://pith.science/api/pith-number/NXALNWLRI3IRNDEGSWNWNZE4OI/events.json","paper":"https://pith.science/paper/NXALNWLR"},"agent_actions":{"view_html":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI","download_json":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI.json","view_paper":"https://pith.science/paper/NXALNWLR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.6618&json=true","fetch_graph":"https://pith.science/api/pith-number/NXALNWLRI3IRNDEGSWNWNZE4OI/graph.json","fetch_events":"https://pith.science/api/pith-number/NXALNWLRI3IRNDEGSWNWNZE4OI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI/action/storage_attestation","attest_author":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI/action/author_attestation","sign_citation":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI/action/citation_signature","submit_replication":"https://pith.science/pith/NXALNWLRI3IRNDEGSWNWNZE4OI/action/replication_record"}},"created_at":"2026-05-18T02:26:45.204498+00:00","updated_at":"2026-05-18T02:26:45.204498+00:00"}