{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:RJPSYIPJJYZIAOLGUF3ZIWW4TW","short_pith_number":"pith:RJPSYIPJ","schema_version":"1.0","canonical_sha256":"8a5f2c21e94e32803966a177945adc9dba78bac6249662a0c4dafeb5fb229cd2","source":{"kind":"arxiv","id":"1903.11820","version":1},"attestation_state":"computed","paper":{"title":"Small field models of inflation that predict a tensor-to-scalar ratio $r=0.03$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Ira Wolfson, Ram Brustein","submitted_at":"2019-03-28T07:54:30Z","abstract_excerpt":"Future observations of the cosmic microwave background (CMB) polarization are expected to set an improved upper bound on the tensor-to-scalar ratio of $r\\lesssim 0.03$. Recently, we showed that small field models of inflation can produce a significant primordial gravitational wave signal. We constructed viable small field models that predict a value of $r$ as high as $0.01$. Models that predict higher values of $r$ are more tightly constrained and lead to larger field excursions. This leads to an increase in tuning of the potential parameters and requires higher levels of error control in the "},"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":"1903.11820","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-03-28T07:54:30Z","cross_cats_sorted":[],"title_canon_sha256":"c922fecde892e8f5ee0e59bb0affb2bc87a56b4f47d0ea0d7da27043a64c3ed3","abstract_canon_sha256":"7e8f63e72875d96dbefdb4cc8c6c5aab634461c4da25cec6498c18f5b42d7d3b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T23:58:47.656965Z","signature_b64":"3HBsPICKayWFhIRYKSnB5lwSSmQSResZ6zs9Oa9pbeKO3M8X4g5JPEHxbNEtScvj3KHX2n5is/IL+RmIaovmAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8a5f2c21e94e32803966a177945adc9dba78bac6249662a0c4dafeb5fb229cd2","last_reissued_at":"2026-07-04T23:58:47.656536Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T23:58:47.656536Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Small field models of inflation that predict a tensor-to-scalar ratio $r=0.03$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Ira Wolfson, Ram Brustein","submitted_at":"2019-03-28T07:54:30Z","abstract_excerpt":"Future observations of the cosmic microwave background (CMB) polarization are expected to set an improved upper bound on the tensor-to-scalar ratio of $r\\lesssim 0.03$. Recently, we showed that small field models of inflation can produce a significant primordial gravitational wave signal. We constructed viable small field models that predict a value of $r$ as high as $0.01$. Models that predict higher values of $r$ are more tightly constrained and lead to larger field excursions. This leads to an increase in tuning of the potential parameters and requires higher levels of error control in the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1903.11820","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/1903.11820/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":"1903.11820","created_at":"2026-07-04T23:58:47.656596+00:00"},{"alias_kind":"arxiv_version","alias_value":"1903.11820v1","created_at":"2026-07-04T23:58:47.656596+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1903.11820","created_at":"2026-07-04T23:58:47.656596+00:00"},{"alias_kind":"pith_short_12","alias_value":"RJPSYIPJJYZI","created_at":"2026-07-04T23:58:47.656596+00:00"},{"alias_kind":"pith_short_16","alias_value":"RJPSYIPJJYZIAOLG","created_at":"2026-07-04T23:58:47.656596+00:00"},{"alias_kind":"pith_short_8","alias_value":"RJPSYIPJ","created_at":"2026-07-04T23:58:47.656596+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1909.00568","citing_title":"B-mode Power Spectrum of CMB via Polarized Compton Scattering","ref_index":50,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW","json":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW.json","graph_json":"https://pith.science/api/pith-number/RJPSYIPJJYZIAOLGUF3ZIWW4TW/graph.json","events_json":"https://pith.science/api/pith-number/RJPSYIPJJYZIAOLGUF3ZIWW4TW/events.json","paper":"https://pith.science/paper/RJPSYIPJ"},"agent_actions":{"view_html":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW","download_json":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW.json","view_paper":"https://pith.science/paper/RJPSYIPJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1903.11820&json=true","fetch_graph":"https://pith.science/api/pith-number/RJPSYIPJJYZIAOLGUF3ZIWW4TW/graph.json","fetch_events":"https://pith.science/api/pith-number/RJPSYIPJJYZIAOLGUF3ZIWW4TW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW/action/storage_attestation","attest_author":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW/action/author_attestation","sign_citation":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW/action/citation_signature","submit_replication":"https://pith.science/pith/RJPSYIPJJYZIAOLGUF3ZIWW4TW/action/replication_record"}},"created_at":"2026-07-04T23:58:47.656596+00:00","updated_at":"2026-07-04T23:58:47.656596+00:00"}