{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:MPK3KYKMJPTKFAEWOZGCEAKBSK","short_pith_number":"pith:MPK3KYKM","schema_version":"1.0","canonical_sha256":"63d5b5614c4be6a28096764c220141928eb117c7e94f5d46c76c4552c7d8c52e","source":{"kind":"arxiv","id":"2304.14260","version":2},"attestation_state":"computed","paper":{"title":"Multi-field inflation with large scalar fluctuations: non-Gaussianity and perturbativity","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"David J. Mulryne, Laura Iacconi","submitted_at":"2023-04-27T15:16:55Z","abstract_excerpt":"Recently multi-field inflation models that can produce large scalar fluctuations on small scales have drawn a lot of attention, primarily because they could lead to primordial black hole production and generation of large second-order gravitational waves. In this work, we focus on models where the scalar fields responsible for inflation live on a hyperbolic field space. In this case, geometrical destabilisation and non-geodesic motion are responsible for the peak in the scalar power spectrum. We present new results for scalar non-Gaussianity and discuss its dependence on the model's parameters"},"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":"2304.14260","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-04-27T15:16:55Z","cross_cats_sorted":["gr-qc","hep-ph","hep-th"],"title_canon_sha256":"e8b1d0a12df1889fa9cb9c318f5f37e2dfba7e13458475342d70c739f957c1db","abstract_canon_sha256":"77658b508854a2e7eb8116dc35356ef02693f995705cbf0d5add229e10eaab4c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:52:22.955308Z","signature_b64":"E7r7dqyqB39PGg91KqncVTxyAU+opbkyQFj/E4t0rDUAH9WbTFeFxZ7kBGcoAH4uunFanXFlWaKQlvHx/2IrBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"63d5b5614c4be6a28096764c220141928eb117c7e94f5d46c76c4552c7d8c52e","last_reissued_at":"2026-07-05T06:52:22.954803Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:52:22.954803Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Multi-field inflation with large scalar fluctuations: non-Gaussianity and perturbativity","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"David J. Mulryne, Laura Iacconi","submitted_at":"2023-04-27T15:16:55Z","abstract_excerpt":"Recently multi-field inflation models that can produce large scalar fluctuations on small scales have drawn a lot of attention, primarily because they could lead to primordial black hole production and generation of large second-order gravitational waves. In this work, we focus on models where the scalar fields responsible for inflation live on a hyperbolic field space. In this case, geometrical destabilisation and non-geodesic motion are responsible for the peak in the scalar power spectrum. We present new results for scalar non-Gaussianity and discuss its dependence on the model's parameters"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2304.14260","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2304.14260/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":"2304.14260","created_at":"2026-07-05T06:52:22.954867+00:00"},{"alias_kind":"arxiv_version","alias_value":"2304.14260v2","created_at":"2026-07-05T06:52:22.954867+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2304.14260","created_at":"2026-07-05T06:52:22.954867+00:00"},{"alias_kind":"pith_short_12","alias_value":"MPK3KYKMJPTK","created_at":"2026-07-05T06:52:22.954867+00:00"},{"alias_kind":"pith_short_16","alias_value":"MPK3KYKMJPTKFAEW","created_at":"2026-07-05T06:52:22.954867+00:00"},{"alias_kind":"pith_short_8","alias_value":"MPK3KYKM","created_at":"2026-07-05T06:52:22.954867+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2502.09481","citing_title":"Non-Perturbative Hamiltonian and Higher Loop Corrections in USR Inflation","ref_index":43,"is_internal_anchor":false},{"citing_arxiv_id":"2502.10287","citing_title":"Hamiltonians to all Orders in Perturbation Theory and Higher Loop Corrections in Single Field Inflation with PBHs Formation","ref_index":31,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK","json":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK.json","graph_json":"https://pith.science/api/pith-number/MPK3KYKMJPTKFAEWOZGCEAKBSK/graph.json","events_json":"https://pith.science/api/pith-number/MPK3KYKMJPTKFAEWOZGCEAKBSK/events.json","paper":"https://pith.science/paper/MPK3KYKM"},"agent_actions":{"view_html":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK","download_json":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK.json","view_paper":"https://pith.science/paper/MPK3KYKM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2304.14260&json=true","fetch_graph":"https://pith.science/api/pith-number/MPK3KYKMJPTKFAEWOZGCEAKBSK/graph.json","fetch_events":"https://pith.science/api/pith-number/MPK3KYKMJPTKFAEWOZGCEAKBSK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK/action/storage_attestation","attest_author":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK/action/author_attestation","sign_citation":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK/action/citation_signature","submit_replication":"https://pith.science/pith/MPK3KYKMJPTKFAEWOZGCEAKBSK/action/replication_record"}},"created_at":"2026-07-05T06:52:22.954867+00:00","updated_at":"2026-07-05T06:52:22.954867+00:00"}